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</div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.00916">arXiv:2308.00916</a> <span> [<a href="https://arxiv.org/pdf/2308.00916">pdf</a>, <a href="https://arxiv.org/format/2308.00916">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Cosmological Distance Measurement of 12 Nearby Supernovae IIP with ROTSE-IIIB </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dhungana%2C+G">Govinda Dhungana</a>, <a href="/search/astro-ph?searchtype=author&query=Kehoe%2C+R">Robert Kehoe</a>, <a href="/search/astro-ph?searchtype=author&query=Staten%2C+R">Ryan Staten</a>, <a href="/search/astro-ph?searchtype=author&query=Vinko%2C+J">Jozsef Vinko</a>, <a href="/search/astro-ph?searchtype=author&query=Wheeler%2C+J+C">J. Craig Wheeler</a>, <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">Carl W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Doss%2C+D">David Doss</a>, <a href="/search/astro-ph?searchtype=author&query=Farrente%2C+F+V">Farley V. Farrente</a>, <a href="/search/astro-ph?searchtype=author&query=Gibson%2C+C+A">Coyne A. Gibson</a>, <a href="/search/astro-ph?searchtype=author&query=Lasker%2C+J">James Lasker</a>, <a href="/search/astro-ph?searchtype=author&query=Marion%2C+G+H">G. H. Marion</a>, <a href="/search/astro-ph?searchtype=author&query=Pandey%2C+S+B">Shashi Bhushan Pandey</a>, <a href="/search/astro-ph?searchtype=author&query=Quimby%2C+R">Robert Quimby</a>, <a href="/search/astro-ph?searchtype=author&query=Rykoff%2C+E">Eli Rykoff</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+D+A">Donald A. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+F">Fang Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Zheng%2C+W">WeiKang Zheng</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2308.00916v2-abstract-short" style="display: inline;"> We present cosmological analysis of 12 nearby ($z<0.06$) Type IIP supernovae (SNe IIP) observed with the ROTSE-IIIb telescope. To achieve precise photometry, we present a new image differencing technique that is implemented for the first time on the ROTSE SN photometry pipeline. With this method, we find up to a 20\% increase in the detection efficiency and significant reduction in residual RMS sc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.00916v2-abstract-full').style.display = 'inline'; document.getElementById('2308.00916v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.00916v2-abstract-full" style="display: none;"> We present cosmological analysis of 12 nearby ($z<0.06$) Type IIP supernovae (SNe IIP) observed with the ROTSE-IIIb telescope. To achieve precise photometry, we present a new image differencing technique that is implemented for the first time on the ROTSE SN photometry pipeline. With this method, we find up to a 20\% increase in the detection efficiency and significant reduction in residual RMS scatter of the SN lightcurves when compared to the previous pipeline performance. We use the published optical spectra and broadband photometry of well studied SNe IIP to establish temporal models for ejecta velocity and photospheric temperature evolution for our SNe IIP population. This study yields measurements that are competitive to other methods even when the data are limited to a single epoch during the photospheric phase of SNe IIP. Using the fully reduced ROTSE photometry and optical spectra, we apply these models to the respective photometric epochs for each SN in the ROTSE IIP sample. This facilitates the use of the Expanding Photosphere Method (EPM) to obtain distance estimates to their respective host galaxies. We then perform cosmological parameter fitting using these EPM distances from which we measure the Hubble constant to be $72.9^{+5.7}_{-4.3}~{\rm kms^{-1}~Mpc^{-1}}$, which is consistent with the standard $螞CDM$ model values derived using other independent techniques. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.00916v2-abstract-full').style.display = 'none'; document.getElementById('2308.00916v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 13 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.03764">arXiv:2207.03764</a> <span> [<a href="https://arxiv.org/pdf/2207.03764">pdf</a>, <a href="https://arxiv.org/format/2207.03764">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.131.041002">10.1103/PhysRevLett.131.041002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First Dark Matter Search Results from the LUX-ZEPLIN (LZ) Experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Aalbers%2C+J">J. Aalbers</a>, <a href="/search/astro-ph?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Musalhi%2C+A+K+A">A. K. Al Musalhi</a>, <a href="/search/astro-ph?searchtype=author&query=Alder%2C+F">F. Alder</a>, <a href="/search/astro-ph?searchtype=author&query=Alqahtani%2C+A">A. Alqahtani</a>, <a href="/search/astro-ph?searchtype=author&query=Alsum%2C+S+K">S. K. Alsum</a>, <a href="/search/astro-ph?searchtype=author&query=Amarasinghe%2C+C+S">C. S. Amarasinghe</a>, <a href="/search/astro-ph?searchtype=author&query=Ames%2C+A">A. Ames</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+T+J">T. J. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/astro-ph?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+J+E">J. E. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/astro-ph?searchtype=author&query=Azadi%2C+S">S. Azadi</a>, <a href="/search/astro-ph?searchtype=author&query=Bailey%2C+A+J">A. J. Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Baker%2C+A">A. Baker</a>, <a href="/search/astro-ph?searchtype=author&query=Balajthy%2C+J">J. Balajthy</a>, <a href="/search/astro-ph?searchtype=author&query=Balashov%2C+S">S. Balashov</a>, <a href="/search/astro-ph?searchtype=author&query=Bang%2C+J">J. Bang</a>, <a href="/search/astro-ph?searchtype=author&query=Bargemann%2C+J+W">J. W. Bargemann</a>, <a href="/search/astro-ph?searchtype=author&query=Barry%2C+M+J">M. J. Barry</a>, <a href="/search/astro-ph?searchtype=author&query=Barthel%2C+J">J. Barthel</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+D">D. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Baxter%2C+A">A. Baxter</a> , et al. (322 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2207.03764v4-abstract-short" style="display: inline;"> The LUX-ZEPLIN experiment is a dark matter detector centered on a dual-phase xenon time projection chamber operating at the Sanford Underground Research Facility in Lead, South Dakota, USA. This Letter reports results from LUX-ZEPLIN's first search for weakly interacting massive particles (WIMPs) with an exposure of 60~live days using a fiducial mass of 5.5 t. A profile-likelihood ratio analysis s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.03764v4-abstract-full').style.display = 'inline'; document.getElementById('2207.03764v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.03764v4-abstract-full" style="display: none;"> The LUX-ZEPLIN experiment is a dark matter detector centered on a dual-phase xenon time projection chamber operating at the Sanford Underground Research Facility in Lead, South Dakota, USA. This Letter reports results from LUX-ZEPLIN's first search for weakly interacting massive particles (WIMPs) with an exposure of 60~live days using a fiducial mass of 5.5 t. A profile-likelihood ratio analysis shows the data to be consistent with a background-only hypothesis, setting new limits on spin-independent WIMP-nucleon, spin-dependent WIMP-neutron, and spin-dependent WIMP-proton cross sections for WIMP masses above 9 GeV/c$^2$. The most stringent limit is set for spin-independent scattering at 36 GeV/c$^2$, rejecting cross sections above 9.2$\times 10^{-48}$ cm$^2$ at the 90% confidence level. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.03764v4-abstract-full').style.display = 'none'; document.getElementById('2207.03764v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 8 figures. See https://doi.org/10.1103/PhysRevLett.131.041002 for a data release related to this paper</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 131, 041002 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1910.09124">arXiv:1910.09124</a> <span> [<a href="https://arxiv.org/pdf/1910.09124">pdf</a>, <a href="https://arxiv.org/format/1910.09124">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.nima.2019.163047">10.1016/j.nima.2019.163047 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The LUX-ZEPLIN (LZ) Experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+LZ+Collaboration"> The LZ Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Akimov%2C+D+Y">D. Yu. Akimov</a>, <a href="/search/astro-ph?searchtype=author&query=Alquahtani%2C+A">A. Alquahtani</a>, <a href="/search/astro-ph?searchtype=author&query=Alsum%2C+S+K">S. K. Alsum</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+T+J">T. J. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Angelides%2C+N">N. Angelides</a>, <a href="/search/astro-ph?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/astro-ph?searchtype=author&query=Arbuckle%2C+A">A. Arbuckle</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+J+E">J. E. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/astro-ph?searchtype=author&query=Auyeung%2C+H">H. Auyeung</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=Bailey%2C+A+J">A. J. Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Balajthy%2C+J">J. Balajthy</a>, <a href="/search/astro-ph?searchtype=author&query=Balashov%2C+S">S. Balashov</a>, <a href="/search/astro-ph?searchtype=author&query=Bang%2C+J">J. Bang</a>, <a href="/search/astro-ph?searchtype=author&query=Barry%2C+M+J">M. J. Barry</a>, <a href="/search/astro-ph?searchtype=author&query=Barthel%2C+J">J. Barthel</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+D">D. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+P">P. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Baxter%2C+A">A. Baxter</a>, <a href="/search/astro-ph?searchtype=author&query=Belle%2C+J">J. Belle</a>, <a href="/search/astro-ph?searchtype=author&query=Beltrame%2C+P">P. Beltrame</a> , et al. (357 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1910.09124v2-abstract-short" style="display: inline;"> We describe the design and assembly of the LUX-ZEPLIN experiment, a direct detection search for cosmic WIMP dark matter particles. The centerpiece of the experiment is a large liquid xenon time projection chamber sensitive to low energy nuclear recoils. Rejection of backgrounds is enhanced by a Xe skin veto detector and by a liquid scintillator Outer Detector loaded with gadolinium for efficient n… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.09124v2-abstract-full').style.display = 'inline'; document.getElementById('1910.09124v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1910.09124v2-abstract-full" style="display: none;"> We describe the design and assembly of the LUX-ZEPLIN experiment, a direct detection search for cosmic WIMP dark matter particles. The centerpiece of the experiment is a large liquid xenon time projection chamber sensitive to low energy nuclear recoils. Rejection of backgrounds is enhanced by a Xe skin veto detector and by a liquid scintillator Outer Detector loaded with gadolinium for efficient neutron capture and tagging. LZ is located in the Davis Cavern at the 4850' level of the Sanford Underground Research Facility in Lead, South Dakota, USA. We describe the major subsystems of the experiment and its key design features and requirements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.09124v2-abstract-full').style.display = 'none'; document.getElementById('1910.09124v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 November, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 October, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2019. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1802.06039">arXiv:1802.06039</a> <span> [<a href="https://arxiv.org/pdf/1802.06039">pdf</a>, <a href="https://arxiv.org/format/1802.06039">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.101.052002">10.1103/PhysRevD.101.052002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Projected WIMP sensitivity of the LUX-ZEPLIN (LZ) dark matter experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Alsum%2C+S+K">S. K. Alsum</a>, <a href="/search/astro-ph?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/astro-ph?searchtype=author&query=Arthurs%2C+M">M. Arthurs</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=Bailey%2C+A+J">A. J. Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Balajthy%2C+J">J. Balajthy</a>, <a href="/search/astro-ph?searchtype=author&query=Balashov%2C+S">S. Balashov</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+D">D. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Belle%2C+J">J. Belle</a>, <a href="/search/astro-ph?searchtype=author&query=Beltrame%2C+P">P. Beltrame</a>, <a href="/search/astro-ph?searchtype=author&query=Benson%2C+T">T. Benson</a>, <a href="/search/astro-ph?searchtype=author&query=Bernard%2C+E+P">E. P. Bernard</a>, <a href="/search/astro-ph?searchtype=author&query=Biesiadzinski%2C+T+P">T. P. Biesiadzinski</a>, <a href="/search/astro-ph?searchtype=author&query=Boast%2C+K+E">K. E. Boast</a>, <a href="/search/astro-ph?searchtype=author&query=Boxer%2C+B">B. Boxer</a>, <a href="/search/astro-ph?searchtype=author&query=Br%C3%A1s%2C+P">P. Br谩s</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+J+H">J. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Bugaev%2C+V+V">V. V. Bugaev</a>, <a href="/search/astro-ph?searchtype=author&query=Burdin%2C+S">S. Burdin</a>, <a href="/search/astro-ph?searchtype=author&query=Busenitz%2C+J+K">J. K. Busenitz</a>, <a href="/search/astro-ph?searchtype=author&query=Carels%2C+C">C. Carels</a>, <a href="/search/astro-ph?searchtype=author&query=Carlsmith%2C+D+L">D. L. Carlsmith</a>, <a href="/search/astro-ph?searchtype=author&query=Carlson%2C+B">B. Carlson</a> , et al. (153 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1802.06039v2-abstract-short" style="display: inline;"> LUX-ZEPLIN (LZ) is a next generation dark matter direct detection experiment that will operate 4850 feet underground at the Sanford Underground Research Facility (SURF) in Lead, South Dakota, USA. Using a two-phase xenon detector with an active mass of 7~tonnes, LZ will search primarily for low-energy interactions with Weakly Interacting Massive Particles (WIMPs), which are hypothesized to make up… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.06039v2-abstract-full').style.display = 'inline'; document.getElementById('1802.06039v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1802.06039v2-abstract-full" style="display: none;"> LUX-ZEPLIN (LZ) is a next generation dark matter direct detection experiment that will operate 4850 feet underground at the Sanford Underground Research Facility (SURF) in Lead, South Dakota, USA. Using a two-phase xenon detector with an active mass of 7~tonnes, LZ will search primarily for low-energy interactions with Weakly Interacting Massive Particles (WIMPs), which are hypothesized to make up the dark matter in our galactic halo. In this paper, the projected WIMP sensitivity of LZ is presented based on the latest background estimates and simulations of the detector. For a 1000~live day run using a 5.6~tonne fiducial mass, LZ is projected to exclude at 90\% confidence level spin-independent WIMP-nucleon cross sections above $1.4 \times 10^{-48}$~cm$^{2}$ for a 40~$\mathrm{GeV}/c^{2}$ mass WIMP. Additionally, a $5蟽$ discovery potential is projected reaching cross sections below the exclusion limits of recent experiments. For spin-dependent WIMP-neutron(-proton) scattering, a sensitivity of $2.3 \times 10^{-43}$~cm$^{2}$ ($7.1 \times 10^{-42}$~cm$^{2}$) for a 40~$\mathrm{GeV}/c^{2}$ mass WIMP is expected. With underground installation well underway, LZ is on track for commissioning at SURF in 2020. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.06039v2-abstract-full').style.display = 'none'; document.getElementById('1802.06039v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 December, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 February, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 11 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 101, 052002 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1703.09144">arXiv:1703.09144</a> <span> [<a href="https://arxiv.org/pdf/1703.09144">pdf</a>, <a href="https://arxiv.org/format/1703.09144">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> LUX-ZEPLIN (LZ) Technical Design Report </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mount%2C+B+J">B. J. Mount</a>, <a href="/search/astro-ph?searchtype=author&query=Hans%2C+S">S. Hans</a>, <a href="/search/astro-ph?searchtype=author&query=Rosero%2C+R">R. Rosero</a>, <a href="/search/astro-ph?searchtype=author&query=Yeh%2C+M">M. Yeh</a>, <a href="/search/astro-ph?searchtype=author&query=Chan%2C+C">C. Chan</a>, <a href="/search/astro-ph?searchtype=author&query=Gaitskell%2C+R+J">R. J. Gaitskell</a>, <a href="/search/astro-ph?searchtype=author&query=Huang%2C+D+Q">D. Q. Huang</a>, <a href="/search/astro-ph?searchtype=author&query=Makkinje%2C+J">J. Makkinje</a>, <a href="/search/astro-ph?searchtype=author&query=Malling%2C+D+C">D. C. Malling</a>, <a href="/search/astro-ph?searchtype=author&query=Pangilinan%2C+M">M. Pangilinan</a>, <a href="/search/astro-ph?searchtype=author&query=Rhyne%2C+C+A">C. A. Rhyne</a>, <a href="/search/astro-ph?searchtype=author&query=Taylor%2C+W+C">W. C. Taylor</a>, <a href="/search/astro-ph?searchtype=author&query=Verbus%2C+J+R">J. R. Verbus</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+Y+D">Y. D. Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+H+S">H. S. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J">J. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Leonard%2C+D+S">D. S. Leonard</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+J">J. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Belle%2C+J">J. Belle</a>, <a href="/search/astro-ph?searchtype=author&query=Cottle%2C+A">A. Cottle</a>, <a href="/search/astro-ph?searchtype=author&query=Lippincott%2C+W+H">W. H. Lippincott</a>, <a href="/search/astro-ph?searchtype=author&query=Markley%2C+D+J">D. J. Markley</a>, <a href="/search/astro-ph?searchtype=author&query=Martin%2C+T+J">T. J. Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Sarychev%2C+M">M. Sarychev</a>, <a href="/search/astro-ph?searchtype=author&query=Tope%2C+T+E">T. E. Tope</a> , et al. (237 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1703.09144v1-abstract-short" style="display: inline;"> In this Technical Design Report (TDR) we describe the LZ detector to be built at the Sanford Underground Research Facility (SURF). The LZ dark matter experiment is designed to achieve sensitivity to a WIMP-nucleon spin-independent cross section of three times ten to the negative forty-eighth square centimeters. </span> <span class="abstract-full has-text-grey-dark mathjax" id="1703.09144v1-abstract-full" style="display: none;"> In this Technical Design Report (TDR) we describe the LZ detector to be built at the Sanford Underground Research Facility (SURF). The LZ dark matter experiment is designed to achieve sensitivity to a WIMP-nucleon spin-independent cross section of three times ten to the negative forty-eighth square centimeters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.09144v1-abstract-full').style.display = 'none'; document.getElementById('1703.09144v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 March, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">392 pages. Submitted to the Department of Energy as part of the documentation for the Critical Decision Numbers Two and Three (CD-2 and CD-3) management processes. Report also available by chapter at <a href="http://hep.ucsb.edu/LZ/TDR/">this URL</a></span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LBNL-1007256 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1509.02910">arXiv:1509.02910</a> <span> [<a href="https://arxiv.org/pdf/1509.02910">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> LUX-ZEPLIN (LZ) Conceptual Design Report </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+LZ+Collaboration"> The LZ Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Akerib%2C+D+S">D. S. Akerib</a>, <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Akimov%2C+D+Y">D. Yu. Akimov</a>, <a href="/search/astro-ph?searchtype=author&query=Alsum%2C+S+K">S. K. Alsum</a>, <a href="/search/astro-ph?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M. Ara煤jo</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=Bailey%2C+A+J">A. J. Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Balajthy%2C+J">J. Balajthy</a>, <a href="/search/astro-ph?searchtype=author&query=Balashov%2C+S">S. Balashov</a>, <a href="/search/astro-ph?searchtype=author&query=Barry%2C+M+J">M. J. Barry</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+P">P. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Beltrame%2C+P">P. Beltrame</a>, <a href="/search/astro-ph?searchtype=author&query=Bernard%2C+E+P">E. P. Bernard</a>, <a href="/search/astro-ph?searchtype=author&query=Bernstein%2C+A">A. Bernstein</a>, <a href="/search/astro-ph?searchtype=author&query=Biesiadzinski%2C+T+P">T. P. Biesiadzinski</a>, <a href="/search/astro-ph?searchtype=author&query=Boast%2C+K+E">K. E. Boast</a>, <a href="/search/astro-ph?searchtype=author&query=Bolozdynya%2C+A+I">A. I. Bolozdynya</a>, <a href="/search/astro-ph?searchtype=author&query=Boulton%2C+E+M">E. M. Boulton</a>, <a href="/search/astro-ph?searchtype=author&query=Bramante%2C+R">R. Bramante</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+J+H">J. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Bugaev%2C+V+V">V. V. Bugaev</a>, <a href="/search/astro-ph?searchtype=author&query=Bunker%2C+R">R. Bunker</a>, <a href="/search/astro-ph?searchtype=author&query=Burdin%2C+S">S. Burdin</a>, <a href="/search/astro-ph?searchtype=author&query=Busenitz%2C+J+K">J. K. Busenitz</a> , et al. (170 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1509.02910v2-abstract-short" style="display: inline;"> The design and performance of the LUX-ZEPLIN (LZ) detector is described as of March 2015 in this Conceptual Design Report. LZ is a second-generation dark-matter detector with the potential for unprecedented sensitivity to weakly interacting massive particles (WIMPs) of masses from a few GeV/c2 to hundreds of TeV/c2. With total liquid xenon mass of about 10 tonnes, LZ will be the most sensitive exp… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.02910v2-abstract-full').style.display = 'inline'; document.getElementById('1509.02910v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1509.02910v2-abstract-full" style="display: none;"> The design and performance of the LUX-ZEPLIN (LZ) detector is described as of March 2015 in this Conceptual Design Report. LZ is a second-generation dark-matter detector with the potential for unprecedented sensitivity to weakly interacting massive particles (WIMPs) of masses from a few GeV/c2 to hundreds of TeV/c2. With total liquid xenon mass of about 10 tonnes, LZ will be the most sensitive experiment for WIMPs in this mass region by the end of the decade. This report describes in detail the design of the LZ technical systems. Expected backgrounds are quantified and the performance of the experiment is presented. The LZ detector will be located at the Sanford Underground Research Facility in South Dakota. The organization of the LZ Project and a summary of the expected cost and current schedule are given. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.02910v2-abstract-full').style.display = 'none'; document.getElementById('1509.02910v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 September, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 September, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">278 pages. Submitted to the Department of Energy as part of the documentation for the Critical Decision Number One (CD-1) management process. Report also available by chapter at http://hep.ucsb.edu/LZ/CDR. This version includes corrections of minor typographic errors</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LBNL-190005 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1409.4189">arXiv:1409.4189</a> <span> [<a href="https://arxiv.org/pdf/1409.4189">pdf</a>, <a href="https://arxiv.org/ps/1409.4189">ps</a>, <a href="https://arxiv.org/format/1409.4189">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/795/2/103">10.1088/0004-637X/795/2/103 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Optical Luminosity Function of Gamma-ray Bursts deduced from ROTSE-III Observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cui%2C+X+H">X. H. Cui</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+X+F">X. F. Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Wei%2C+J+J">J. J. Wei</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+F">F. Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Zheng%2C+W+K">W. K. Zheng</a>, <a href="/search/astro-ph?searchtype=author&query=Liang%2C+E+W">E. W. Liang</a>, <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Ashley%2C+M+C+B">M. C. B. Ashley</a>, <a href="/search/astro-ph?searchtype=author&query=Flewelling%2C+H+A">H. A. Flewelling</a>, <a href="/search/astro-ph?searchtype=author&query=Gogus%2C+E">E. Gogus</a>, <a href="/search/astro-ph?searchtype=author&query=Guver%2C+T">T. Guver</a>, <a href="/search/astro-ph?searchtype=author&query=Kiziloglu%2C+U">U. Kiziloglu</a>, <a href="/search/astro-ph?searchtype=author&query=McKay%2C+T+A">T. A. McKay</a>, <a href="/search/astro-ph?searchtype=author&query=Pandey%2C+S+B">S. B. Pandey</a>, <a href="/search/astro-ph?searchtype=author&query=Rykoff%2C+E+S">E. S. Rykoff</a>, <a href="/search/astro-ph?searchtype=author&query=Rujopakarn%2C+W">W. Rujopakarn</a>, <a href="/search/astro-ph?searchtype=author&query=Schaefer%2C+B+E">B. E. Schaefer</a>, <a href="/search/astro-ph?searchtype=author&query=Wheeler%2C+J+C">J. C. Wheeler</a>, <a href="/search/astro-ph?searchtype=author&query=Yost%2C+S+A">S. A. Yost</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1409.4189v1-abstract-short" style="display: inline;"> We present the optical luminosity function (LF) of gamma-ray bursts (GRBs) estimated from a uniform sample of 58 GRBs from observations with the Robotic Optical Transient Search Experiment III (ROTSE-III). Our GRB sample is divided into two sub-samples: detected afterglows (18 GRBs), and those with upper limits (40 GRBs). The $R$ band fluxes 100s after the onset of the burst for these two sub-samp… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1409.4189v1-abstract-full').style.display = 'inline'; document.getElementById('1409.4189v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1409.4189v1-abstract-full" style="display: none;"> We present the optical luminosity function (LF) of gamma-ray bursts (GRBs) estimated from a uniform sample of 58 GRBs from observations with the Robotic Optical Transient Search Experiment III (ROTSE-III). Our GRB sample is divided into two sub-samples: detected afterglows (18 GRBs), and those with upper limits (40 GRBs). The $R$ band fluxes 100s after the onset of the burst for these two sub-samples are derived. The optical LFs at 100s are fitted by assuming that the co-moving GRB rate traces the star-formation rate. The detection function of ROTSE-III is taken into account during the fitting of the optical LFs by using Monte Carlo simulations. We find that the cumulative distribution of optical emission at 100s is well-described with an exponential rise and power-law decay (ERPLD), broken power-law (BPL), and Schechter LFs. A single power-law (SPL) LF, on the other hand, is ruled out with high confidence. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1409.4189v1-abstract-full').style.display = 'none'; document.getElementById('1409.4189v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 September, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">26 pages, 3 figures, ApJ accepted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1405.3114">arXiv:1405.3114</a> <span> [<a href="https://arxiv.org/pdf/1405.3114">pdf</a>, <a href="https://arxiv.org/format/1405.3114">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201423920">10.1051/0004-6361/201423920 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Trio of GRB-SNe: GRB 120729A, GRB 130215A / SN 2013ez and GRB 130831A / SN 2013fu </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cano%2C+Z">Z. Cano</a>, <a href="/search/astro-ph?searchtype=author&query=Postigo%2C+A+d+U">A. de Ugarte Postigo</a>, <a href="/search/astro-ph?searchtype=author&query=Pozanenko%2C+A">A. Pozanenko</a>, <a href="/search/astro-ph?searchtype=author&query=Butler%2C+N">N. Butler</a>, <a href="/search/astro-ph?searchtype=author&query=Thone%2C+C+C">C. C. Thone</a>, <a href="/search/astro-ph?searchtype=author&query=Guidorzi%2C+C">C. Guidorzi</a>, <a href="/search/astro-ph?searchtype=author&query=Kruhler%2C+T">T. Kruhler</a>, <a href="/search/astro-ph?searchtype=author&query=Gorosabel%2C+J">J. Gorosabel</a>, <a href="/search/astro-ph?searchtype=author&query=Jakobsson%2C+P">P. Jakobsson</a>, <a href="/search/astro-ph?searchtype=author&query=Leloudas%2C+G">G. Leloudas</a>, <a href="/search/astro-ph?searchtype=author&query=Malesani%2C+D">D. Malesani</a>, <a href="/search/astro-ph?searchtype=author&query=Hjorth%2C+J">J. Hjorth</a>, <a href="/search/astro-ph?searchtype=author&query=Melandri%2C+A">A. Melandri</a>, <a href="/search/astro-ph?searchtype=author&query=Mundell%2C+C">C. Mundell</a>, <a href="/search/astro-ph?searchtype=author&query=Wiersema%2C+K">K. Wiersema</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Avanzo%2C+P">P. D'Avanzo</a>, <a href="/search/astro-ph?searchtype=author&query=Schulze%2C+S">S. Schulze</a>, <a href="/search/astro-ph?searchtype=author&query=Gomboc%2C+A">A. Gomboc</a>, <a href="/search/astro-ph?searchtype=author&query=Johansson%2C+A">A. Johansson</a>, <a href="/search/astro-ph?searchtype=author&query=Zheng%2C+W">W. Zheng</a>, <a href="/search/astro-ph?searchtype=author&query=Kann%2C+D+A">D. A. Kann</a>, <a href="/search/astro-ph?searchtype=author&query=Knust%2C+F">F. Knust</a>, <a href="/search/astro-ph?searchtype=author&query=Varela%2C+K">K. Varela</a>, <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Bloom%2C+J">J. Bloom</a> , et al. (40 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1405.3114v1-abstract-short" style="display: inline;"> We present optical and near-infrared (NIR) photometry for three gamma-ray burst supernovae (GRB-SNe): GRB 120729A, GRB 130215A / SN 2013ez and GRB 130831A / SN 2013fu. In the case of GRB 130215A / SN 2013ez, we also present optical spectroscopy at t-t0=16.1 d, which covers rest-frame 3000-6250 Angstroms. Based on Fe II (5169) and Si (II) (6355), our spectrum indicates an unusually low expansion ve… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1405.3114v1-abstract-full').style.display = 'inline'; document.getElementById('1405.3114v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1405.3114v1-abstract-full" style="display: none;"> We present optical and near-infrared (NIR) photometry for three gamma-ray burst supernovae (GRB-SNe): GRB 120729A, GRB 130215A / SN 2013ez and GRB 130831A / SN 2013fu. In the case of GRB 130215A / SN 2013ez, we also present optical spectroscopy at t-t0=16.1 d, which covers rest-frame 3000-6250 Angstroms. Based on Fe II (5169) and Si (II) (6355), our spectrum indicates an unusually low expansion velocity of 4000-6350 km/s, the lowest ever measured for a GRB-SN. Additionally, we determined the brightness and shape of each accompanying SN relative to a template supernova (SN 1998bw), which were used to estimate the amount of nickel produced via nucleosynthesis during each explosion. We find that our derived nickel masses are typical of other GRB-SNe, and greater than those of SNe Ibc that are not associated with GRBs. For GRB 130831A / SN 2013fu, we use our well-sampled R-band light curve (LC) to estimate the amount of ejecta mass and the kinetic energy of the SN, finding that these too are similar to other GRB-SNe. For GRB 130215A, we take advantage of contemporaneous optical/NIR observations to construct an optical/NIR bolometric LC of the afterglow. We fit the bolometric LC with the millisecond magnetar model of Zhang & Meszaros (2001), which considers dipole radiation as a source of energy injection to the forward shock powering the optical/NIR afterglow. Using this model we derive an initial spin period of P=12 ms and a magnetic field of B=1.1 x 10^15 G, which are commensurate with those found for proposed magnetar central engines of other long-duration GRBs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1405.3114v1-abstract-full').style.display = 'none'; document.getElementById('1405.3114v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 May, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Archive copy - 24 pages, 12 Figures, 3 Tables. Submitted to A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 568, A19 (2014) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1205.3066">arXiv:1205.3066</a> <span> [<a href="https://arxiv.org/pdf/1205.3066">pdf</a>, <a href="https://arxiv.org/ps/1205.3066">ps</a>, <a href="https://arxiv.org/format/1205.3066">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/764/2/190">10.1088/0004-637X/764/2/190 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Limits to the fraction of high-energy photon emitting gamma-ray bursts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">Carl W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Zheng%2C+W">WeiKang Zheng</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1205.3066v2-abstract-short" style="display: inline;"> After almost 4 years of operation, the two instruments onboard the Fermi Gamma-ray Space Telescope have shown that the number of gamma-ray bursts with high energy photon emission above 100 MeV cannot exceed roughly 9% of the total number of all such events, at least at the present detection limits. In a recent paper (Zheng et al. 2012c), we found that GRBs with photons detected in the Large Area T… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1205.3066v2-abstract-full').style.display = 'inline'; document.getElementById('1205.3066v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1205.3066v2-abstract-full" style="display: none;"> After almost 4 years of operation, the two instruments onboard the Fermi Gamma-ray Space Telescope have shown that the number of gamma-ray bursts with high energy photon emission above 100 MeV cannot exceed roughly 9% of the total number of all such events, at least at the present detection limits. In a recent paper (Zheng et al. 2012c), we found that GRBs with photons detected in the Large Area Telescope (LAT) have a surprisingly broad distribution with respect to the photon number above background. Extrapolation of our empirical fit to numbers of photons below our quoted detection limit suggests that the overall rate of such events could be determined by standard image co-adding techniques. In this case, we have taken advantage of the excellent angular resolution of the Swift mission to provide accurate reference points for 79 GRB events which have eluded any previous correlations with high energy photons. We find a small but significant signal. Guided by the power law fit obtained previously for the number distribution of GRBs, the data suggests that only a small fraction of GRBs are sources of high energy photons. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1205.3066v2-abstract-full').style.display = 'none'; document.getElementById('1205.3066v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 January, 2013; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 May, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 3 figures, 2 tables, accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1203.5113">arXiv:1203.5113</a> <span> [<a href="https://arxiv.org/pdf/1203.5113">pdf</a>, <a href="https://arxiv.org/ps/1203.5113">ps</a>, <a href="https://arxiv.org/format/1203.5113">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/756/1/64">10.1088/0004-637X/756/1/64 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> GRB 110709A, 111117A and 120107A: Faint high-energy gamma-ray photon emission from Fermi/LAT observations and demographic implications </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zheng%2C+W">Weikang Zheng</a>, <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">Carl W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Pandey%2C+S+B">Shashi B. Pandey</a>, <a href="/search/astro-ph?searchtype=author&query=McKay%2C+T+A">Timothy A. McKay</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+B">Binbin Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+B">Bing Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Sakamoto%2C+T">Takanori Sakamoto</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1203.5113v2-abstract-short" style="display: inline;"> Launched on June 11, 2008, the LAT instrument onboard the $Fermi$ Gamma-ray Space Telescope has provided a rare opportunity to study high energy photon emission from gamma-ray bursts. Although the majority of such events (27) have been iden tified by the Fermi LAT Collaboration, four were uncovered by using more sensiti ve statistical techniques (Akerlof et al 2010, Akerlof et al 2011, Zheng et al… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1203.5113v2-abstract-full').style.display = 'inline'; document.getElementById('1203.5113v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1203.5113v2-abstract-full" style="display: none;"> Launched on June 11, 2008, the LAT instrument onboard the $Fermi$ Gamma-ray Space Telescope has provided a rare opportunity to study high energy photon emission from gamma-ray bursts. Although the majority of such events (27) have been iden tified by the Fermi LAT Collaboration, four were uncovered by using more sensiti ve statistical techniques (Akerlof et al 2010, Akerlof et al 2011, Zheng et al 2 012). In this paper, we continue our earlier work by finding three more GRBs ass ociated with high energy photon emission, GRB 110709A, 111117A and 120107A. To s ystematize our matched filter approach, a pipeline has been developed to identif y these objects in near real time. GRB 120107A is the first product of this anal ysis procedure. Despite the reduced threshold for identification, the number of GRB events has not increased significantly. This relative dearth of events with low photon number prompted a study of the apparent photon number distribution. W e find an extremely good fit to a simple power-law with an exponent of -1.8 $\pm $ 0.3 for the differential distribution. As might be expected, there is a substa ntial correlation between the number of lower energy photons detected by the GBM and the number observed by the LAT. Thus, high energy photon emission is associ ated with some but not all of the brighter GBM events. Deeper studies of the pro perties of the small population of high energy emitting bursts may eventually yi eld a better understanding of these entire phenomena. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1203.5113v2-abstract-full').style.display = 'none'; document.getElementById('1203.5113v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 July, 2012; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 March, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1201.3844">arXiv:1201.3844</a> <span> [<a href="https://arxiv.org/pdf/1201.3844">pdf</a>, <a href="https://arxiv.org/ps/1201.3844">ps</a>, <a href="https://arxiv.org/format/1201.3844">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/745/1/72">10.1088/0004-637X/745/1/72 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Faint high-energy gamma-ray photon emission of GRB 081006A from Fermi observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zheng%2C+W">WeiKang Zheng</a>, <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">Carl W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Pandey%2C+S+B">Shashi B. Pandey</a>, <a href="/search/astro-ph?searchtype=author&query=McKay%2C+T+A">Timothy A. McKay</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+B">BinBin Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+B">Bing Zhang</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1201.3844v1-abstract-short" style="display: inline;"> Since the launch of the Fermi gamma - ray Space Telescope on June 11, 2008, the LAT instrument has solidly detected more than 20 GRBs with high energy photon emission above 100 MeV. Using the matched filter technique, 3 more GRBs have also shown evidence of correlation with high energy photon emission as demonstrated by Akerlof et al. In this paper, we present another GRB unambiguously detected by… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1201.3844v1-abstract-full').style.display = 'inline'; document.getElementById('1201.3844v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1201.3844v1-abstract-full" style="display: none;"> Since the launch of the Fermi gamma - ray Space Telescope on June 11, 2008, the LAT instrument has solidly detected more than 20 GRBs with high energy photon emission above 100 MeV. Using the matched filter technique, 3 more GRBs have also shown evidence of correlation with high energy photon emission as demonstrated by Akerlof et al. In this paper, we present another GRB unambiguously detected by the matched filter technique, GRB 081006A. This event is associated with more than 13 high energy photons above 100 MeV. The likelihood analysis code provided by the $Fermi$ Science Support Center (FSSC) generated an independent verification of this detection by comparison of the Test Statistics (TS) value with similar calculations for random LAT data fields. We have performed detailed temporal and spectral analysis of photons from 8 keV up to 0.8 GeV from the GBM and the LAT. The properties of GRB 081006A can be compared to the other two long duration GRBs detected at similar significance, GRB 080825C and GRB 090217A. We find that GRB 081006A is more similar to GRB 080825C with comparable appearances of late high energy photon emission. As demonstrated previously, there appears to be a surprising dearth of faint LAT GRBs, with only one additional GRB identified in a sample of 74 GRBs. In this unique period when both $Swift$ and $Fermi$ are operational, there is some urgency to explore this aspect of GRBs as fully as possible. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1201.3844v1-abstract-full').style.display = 'none'; document.getElementById('1201.3844v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 January, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">ApJ, 745, 72</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2012, ApJ, 745, 72 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1111.7030">arXiv:1111.7030</a> <span> [<a href="https://arxiv.org/pdf/1111.7030">pdf</a>, <a href="https://arxiv.org/format/1111.7030">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201118071">10.1051/0004-6361/201118071 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Searching for soft relativistic jets in Core-collapse Supernovae with the IceCube Optical Follow-up Program </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+IceCube+Collaboration"> The IceCube Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abbasi%2C+R">R. Abbasi</a>, <a href="/search/astro-ph?searchtype=author&query=Abdou%2C+Y">Y. Abdou</a>, <a href="/search/astro-ph?searchtype=author&query=Abu-Zayyad%2C+T">T. Abu-Zayyad</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+M+M">M. M. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Altmann%2C+D">D. Altmann</a>, <a href="/search/astro-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/astro-ph?searchtype=author&query=Auffenberg%2C+J">J. Auffenberg</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=Baker%2C+M">M. Baker</a>, <a href="/search/astro-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/astro-ph?searchtype=author&query=Alba%2C+J+L+B">J. L. Bazo Alba</a>, <a href="/search/astro-ph?searchtype=author&query=Beattie%2C+K">K. Beattie</a>, <a href="/search/astro-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/astro-ph?searchtype=author&query=Bechet%2C+S">S. Bechet</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+J+K">J. K. Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+K+-">K. -H. Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Benabderrahmane%2C+M+L">M. L. Benabderrahmane</a>, <a href="/search/astro-ph?searchtype=author&query=BenZvi%2C+S">S. BenZvi</a>, <a href="/search/astro-ph?searchtype=author&query=Berdermann%2C+J">J. Berdermann</a> , et al. (240 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1111.7030v2-abstract-short" style="display: inline;"> Context. Transient neutrino sources such as Gamma-Ray Bursts (GRBs) and Supernovae (SNe) are hypothesized to emit bursts of high-energy neutrinos on a time-scale of \lesssim 100 s. While GRB neutrinos would be produced in high relativistic jets, core-collapse SNe might host soft-relativistic jets, which become stalled in the outer layers of the progenitor star leading to an efficient production of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1111.7030v2-abstract-full').style.display = 'inline'; document.getElementById('1111.7030v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1111.7030v2-abstract-full" style="display: none;"> Context. Transient neutrino sources such as Gamma-Ray Bursts (GRBs) and Supernovae (SNe) are hypothesized to emit bursts of high-energy neutrinos on a time-scale of \lesssim 100 s. While GRB neutrinos would be produced in high relativistic jets, core-collapse SNe might host soft-relativistic jets, which become stalled in the outer layers of the progenitor star leading to an efficient production of high-energy neutrinos. Aims. To increase the sensitivity to these neutrinos and identify their sources, a low-threshold optical follow-up program for neutrino multiplets detected with the IceCube observatory has been implemented. Methods. If a neutrino multiplet, i.e. two or more neutrinos from the same direction within 100 s, is found by IceCube a trigger is sent to the Robotic Optical Transient Search Experiment, ROTSE. The 4 ROTSE telescopes immediately start an observation program of the corresponding region of the sky in order to detect an optical counterpart to the neutrino events. Results. No statistically significant excess in the rate of neutrino multiplets has been observed and furthermore no coincidence with an optical counterpart was found. Conclusion. The search allows, for the first time, to set stringent limits on current models predicting a high-energy neutrino flux from soft relativistic hadronic jets in core-collapse SNe. We conclude that a sub-population of SNe with typical Lorentz boost factor and jet energy of 10 and 3\times10^{51} erg, respectively, does not exceed 4.2% at 90% confidence. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1111.7030v2-abstract-full').style.display = 'none'; document.getElementById('1111.7030v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 December, 2011; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 November, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2011. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 12 figures, submitted to A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 539, A60 (2012) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1111.0283">arXiv:1111.0283</a> <span> [<a href="https://arxiv.org/pdf/1111.0283">pdf</a>, <a href="https://arxiv.org/ps/1111.0283">ps</a>, <a href="https://arxiv.org/format/1111.0283">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/751/2/90">10.1088/0004-637X/751/2/90 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Panchromatic observations of the textbook GRB 110205A: constraining physical mechanisms of prompt emission and afterglow </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zheng%2C+W">W. Zheng</a>, <a href="/search/astro-ph?searchtype=author&query=Shen%2C+R+F">R. F. Shen</a>, <a href="/search/astro-ph?searchtype=author&query=Sakamoto%2C+T">T. Sakamoto</a>, <a href="/search/astro-ph?searchtype=author&query=Beardmore%2C+A+P">A. P. Beardmore</a>, <a href="/search/astro-ph?searchtype=author&query=De+Pasquale%2C+M">M. De Pasquale</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+X+F">X. F. Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Gorosabel%2C+J">J. Gorosabel</a>, <a href="/search/astro-ph?searchtype=author&query=Urata%2C+Y">Y. Urata</a>, <a href="/search/astro-ph?searchtype=author&query=Sugita%2C+S">S. Sugita</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+B">B. Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Pozanenko%2C+A">A. Pozanenko</a>, <a href="/search/astro-ph?searchtype=author&query=Nissinen%2C+M">M. Nissinen</a>, <a href="/search/astro-ph?searchtype=author&query=Sahu%2C+D+K">D. K. Sahu</a>, <a href="/search/astro-ph?searchtype=author&query=Im%2C+M">M. Im</a>, <a href="/search/astro-ph?searchtype=author&query=Ukwatta%2C+T+N">T. N. Ukwatta</a>, <a href="/search/astro-ph?searchtype=author&query=Andreev%2C+M">M. Andreev</a>, <a href="/search/astro-ph?searchtype=author&query=Klunko%2C+E">E. Klunko</a>, <a href="/search/astro-ph?searchtype=author&query=Volnova%2C+A">A. Volnova</a>, <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Anto%2C+P">P. Anto</a>, <a href="/search/astro-ph?searchtype=author&query=Barthelmy%2C+S+D">S. D. Barthelmy</a>, <a href="/search/astro-ph?searchtype=author&query=Breeveld%2C+A">A. Breeveld</a>, <a href="/search/astro-ph?searchtype=author&query=Carsenty%2C+U">U. Carsenty</a>, <a href="/search/astro-ph?searchtype=author&query=Castillo-Carri%27on%2C+S">S. Castillo-Carri'on</a>, <a href="/search/astro-ph?searchtype=author&query=Castro-Tirado%2C+A+J">A. J. Castro-Tirado</a> , et al. (34 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1111.0283v2-abstract-short" style="display: inline;"> We present a comprehensive analysis of a bright, long duration (T90 ~ 257 s) GRB 110205A at redshift z= 2.22. The optical prompt emission was detected by Swift/UVOT, ROTSE-IIIb and BOOTES telescopes when the GRB was still radiating in the gamma-ray band. Nearly 200 s of observations were obtained simultaneously from optical, X-ray to gamma-ray, which makes it one of the exceptional cases to study… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1111.0283v2-abstract-full').style.display = 'inline'; document.getElementById('1111.0283v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1111.0283v2-abstract-full" style="display: none;"> We present a comprehensive analysis of a bright, long duration (T90 ~ 257 s) GRB 110205A at redshift z= 2.22. The optical prompt emission was detected by Swift/UVOT, ROTSE-IIIb and BOOTES telescopes when the GRB was still radiating in the gamma-ray band. Nearly 200 s of observations were obtained simultaneously from optical, X-ray to gamma-ray, which makes it one of the exceptional cases to study the broadband spectral energy distribution across 6 orders of magnitude in energy during the prompt emission phase. By fitting the time resolved prompt spectra, we clearly identify, for the first time, an interesting two-break energy spectrum, roughly consistent with the standard GRB synchrotron emission model in the fast cooling regime. Although the prompt optical emission is brighter than the extrapolation of the best fit X/gamma-ray spectra, it traces the gamma-ray light curve shape, suggesting a relation to the prompt high energy emission. The synchrotron + SSC scenario is disfavored by the data, but the models invoking a pair of internal shocks or having two emission regions can interpret the data well. Shortly after prompt emission (~ 1100 s), a bright (R = 14.0) optical emission hump with very steep rise (alpha ~ 5.5) was observed which we interpret as the emission from the reverse shock. It is the first time that the rising phase of a reverse shock component has been closely observed. The full optical and X-ray afterglow lightcurves can be interpreted within the standard reverse shock (RS) + forward shock (FS) model. In general, the high quality prompt emission and afterglow data allow us to apply the standard fireball shock model to extract valuable information about the GRB including the radiation mechanism, radius of prompt emission R, initial Lorentz factor of the outflow, the composition of the ejecta, as well as the collimation angle and the total energy budget. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1111.0283v2-abstract-full').style.display = 'none'; document.getElementById('1111.0283v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 March, 2012; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 November, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2011. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted by ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1106.2390">arXiv:1106.2390</a> <span> [<a href="https://arxiv.org/pdf/1106.2390">pdf</a>, <a href="https://arxiv.org/ps/1106.2390">ps</a>, <a href="https://arxiv.org/format/1106.2390">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/736/2/76">10.1088/0004-637X/736/2/76 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Sn 2008in - bridging the gap between normal and faint supernovae of type IIP </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Roy%2C+R">Rupak Roy</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+B">Brijesh Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Benetti%2C+S">Stefano Benetti</a>, <a href="/search/astro-ph?searchtype=author&query=Pastorello%2C+A">Andrea Pastorello</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+F">Fang Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+P+J">Peter J. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Immler%2C+S">Stefan Immler</a>, <a href="/search/astro-ph?searchtype=author&query=Fatkhullin%2C+T+A">Timur A. Fatkhullin</a>, <a href="/search/astro-ph?searchtype=author&query=Moskvitin%2C+A+S">Alexander S. Moskvitin</a>, <a href="/search/astro-ph?searchtype=author&query=Maund%2C+J">Justyn Maund</a>, <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">Carl W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Wheeler%2C+J+C">J. Craig Wheeler</a>, <a href="/search/astro-ph?searchtype=author&query=Sokolov%2C+V+V">Vladimir V. Sokolov</a>, <a href="/search/astro-ph?searchtype=author&query=Quimby%2C+R+M">Rorbert M. Quimby</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">Filomena Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+B">Brajesh Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Misra%2C+K">Kuntal Misra</a>, <a href="/search/astro-ph?searchtype=author&query=Pandey%2C+S+B">S. B. Pandey</a>, <a href="/search/astro-ph?searchtype=author&query=Elias-Rosa%2C+N">Nancy Elias-Rosa</a>, <a href="/search/astro-ph?searchtype=author&query=Roming%2C+P+W+A">Peter W. A. Roming</a>, <a href="/search/astro-ph?searchtype=author&query=Sagar%2C+R">Ram Sagar</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1106.2390v1-abstract-short" style="display: inline;"> We present optical photometric and low-resolution spectroscopic observations of the Type II plateau supernova (SN) 2008in, which occurred in the outskirts of the nearly face-on spiral galaxy M 61. Photometric data in the X-rays, ultraviolet and near-infrared bands have been used to characterize this event. The SN field was imaged with the ROTSE-IIIb optical telescope about seven days before the ex… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1106.2390v1-abstract-full').style.display = 'inline'; document.getElementById('1106.2390v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1106.2390v1-abstract-full" style="display: none;"> We present optical photometric and low-resolution spectroscopic observations of the Type II plateau supernova (SN) 2008in, which occurred in the outskirts of the nearly face-on spiral galaxy M 61. Photometric data in the X-rays, ultraviolet and near-infrared bands have been used to characterize this event. The SN field was imaged with the ROTSE-IIIb optical telescope about seven days before the explosion. This allowed us to constrain the epoch of the shock breakout to JD = 2454825.6. The duration of the plateau phase, as derived from the photometric monitoring, was ~ 98 days. The spectra of SN 2008in show a striking resemblance to those of the archetypal low-luminosity IIP SNe 1997D and 1999br. A comparison of ejecta kinematics of SN 2008in with the hydrodynamical simulations of Type IIP SNe by Dessart et al. (2010) indicates that it is a less energetic event (~ 5$\times10^{50}$ erg). However, the light curve indicates that the production of radioactive $^{56}$Ni is significantly higher than that in the low-luminosity SNe. Adopting an interstellar absorption along the SN direction of $A_V$ ~ 0.3 mag and a distance of 13.2 Mpc, we estimated a synthesized Ni mass of ~ 0.015 $M_{\odot}$. Employing semi-analytical formulae (Litvinova & Nadezhin 1985), we derived a pre-SN radius of ~ 126$R_{\odot}$, an explosion energy of ~ 5.4$\times10^{50}$ erg and a total ejected mass of ~ 16.7$M_{\odot}$. The latter indicates that the zero age main-sequence mass of the progenitor did not exceed 20$M_{\odot}$. Considering the above properties of SN 2008in, and its occurrence in a region of sub-solar metallicity ([O/H] ~ 8.44 dex), it is unlikely that fall-back of the ejecta onto a newly formed black hole occurred in SN 2008in. We therefore favor a low-energy explosion scenario of a relatively compact, moderate-mass progenitor star that generates a neutron star. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1106.2390v1-abstract-full').style.display = 'none'; document.getElementById('1106.2390v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 June, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2011. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in the Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1106.0400">arXiv:1106.0400</a> <span> [<a href="https://arxiv.org/pdf/1106.0400">pdf</a>, <a href="https://arxiv.org/ps/1106.0400">ps</a>, <a href="https://arxiv.org/format/1106.0400">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/736/2/159">10.1088/0004-637X/736/2/159 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Real-Time Detection and Rapid Multiwavelength Follow-up Observations of a Highly Subluminous Type II-P Supernova from the Palomar Transient Factory Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gal-Yam%2C+A">Avishay Gal-Yam</a>, <a href="/search/astro-ph?searchtype=author&query=Kasliwal%2C+M+M">Mansi M. Kasliwal</a>, <a href="/search/astro-ph?searchtype=author&query=Arcavi%2C+I">Iair Arcavi</a>, <a href="/search/astro-ph?searchtype=author&query=Green%2C+Y">Yoav Green</a>, <a href="/search/astro-ph?searchtype=author&query=Yaron%2C+O">Ofer Yaron</a>, <a href="/search/astro-ph?searchtype=author&query=Ben-Ami%2C+S">Sagi Ben-Ami</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+D">Dong Xu</a>, <a href="/search/astro-ph?searchtype=author&query=Sternberg%2C+A">Assaf Sternberg</a>, <a href="/search/astro-ph?searchtype=author&query=Quimby%2C+R+M">Robert M. Quimby</a>, <a href="/search/astro-ph?searchtype=author&query=Kulkarni%2C+S+R">Shrinivas R. Kulkarni</a>, <a href="/search/astro-ph?searchtype=author&query=Ofek%2C+E+O">Eran O. Ofek</a>, <a href="/search/astro-ph?searchtype=author&query=Walters%2C+R">Richard Walters</a>, <a href="/search/astro-ph?searchtype=author&query=Nugent%2C+P+E">Peter E. Nugent</a>, <a href="/search/astro-ph?searchtype=author&query=Poznanski%2C+D">Dovi Poznanski</a>, <a href="/search/astro-ph?searchtype=author&query=Bloom%2C+J+S">Joshua S. Bloom</a>, <a href="/search/astro-ph?searchtype=author&query=Cenko%2C+S+B">S. Bradley Cenko</a>, <a href="/search/astro-ph?searchtype=author&query=Filippenko%2C+A+V">Alexei V. Filippenko</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+W">Weidong Li</a>, <a href="/search/astro-ph?searchtype=author&query=Silverman%2C+J">J. Silverman</a>, <a href="/search/astro-ph?searchtype=author&query=Walker%2C+E+S">Emma S. Walker</a>, <a href="/search/astro-ph?searchtype=author&query=Sullivan%2C+M">Mark Sullivan</a>, <a href="/search/astro-ph?searchtype=author&query=Maguire%2C+K">K. Maguire</a>, <a href="/search/astro-ph?searchtype=author&query=Howell%2C+D+A">D. Andrew Howell</a>, <a href="/search/astro-ph?searchtype=author&query=Mazzali%2C+P+A">Paolo A. Mazzali</a>, <a href="/search/astro-ph?searchtype=author&query=Frail%2C+D+A">Dale A. Frail</a> , et al. (7 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1106.0400v1-abstract-short" style="display: inline;"> The Palomar Transient Factory (PTF) is an optical wide-field variability survey carried out using a camera with a 7.8 square degree field of view mounted on the 48-in Oschin Schmidt telescope at Palomar Observatory. One of the key goals of this survey is to conduct high-cadence monitoring of the sky in order to detect optical transient sources shortly after they occur. Here, we describe the real-t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1106.0400v1-abstract-full').style.display = 'inline'; document.getElementById('1106.0400v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1106.0400v1-abstract-full" style="display: none;"> The Palomar Transient Factory (PTF) is an optical wide-field variability survey carried out using a camera with a 7.8 square degree field of view mounted on the 48-in Oschin Schmidt telescope at Palomar Observatory. One of the key goals of this survey is to conduct high-cadence monitoring of the sky in order to detect optical transient sources shortly after they occur. Here, we describe the real-time capabilities of the PTF and our related rapid multiwavelength follow-up programs, extending from the radio to the gamma-ray bands. We present as a case study observations of the optical transient PTF10vdl (SN 2010id), revealed to be a very young core-collapse (Type II-P) supernova having a remarkably low luminosity. Our results demonstrate that the PTF now provides for optical transients the real-time discovery and rapid-response follow-up capabilities previously reserved only for high-energy transients like gamma-ray bursts. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1106.0400v1-abstract-full').style.display = 'none'; document.getElementById('1106.0400v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 June, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2011. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">ApJ, in press; all spectroscopic data available from the Weizmann Institute of Science Experimental Astrophysics Spectroscopy System (WISEASS; http://www.weizmann.ac.il/astrophysics/wiseass/)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ, 736, 159 (2011) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1010.1588">arXiv:1010.1588</a> <span> [<a href="https://arxiv.org/pdf/1010.1588">pdf</a>, <a href="https://arxiv.org/ps/1010.1588">ps</a>, <a href="https://arxiv.org/format/1010.1588">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/2041-8205/725/1/L15">10.1088/2041-8205/725/1/L15 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Searching for Needles in Haystacks - Using the Fermi/GBM to find GRB gamma-rays with the Fermi/LAT Detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Zheng%2C+W">W. Zheng</a>, <a href="/search/astro-ph?searchtype=author&query=Pandey%2C+S+B">S. B. Pandey</a>, <a href="/search/astro-ph?searchtype=author&query=McKay%2C+T+A">T. A. McKay</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1010.1588v2-abstract-short" style="display: inline;"> From the launch of the Fermi Gamma-ray Space Telescope to July 9, 2010, the Gamma-ray Burst Monitor (GBM) has detected 497 probable GRB events. Twenty-two of these satisfy the simultaneous requirements of an estimated burst direction within 52^\circ of the Fermi Large Area Telescope (LAT) boresight and a low energy fluence exceeding 5 $渭$erg/cm^2. Using matched filter techniques, the spatially cor… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1010.1588v2-abstract-full').style.display = 'inline'; document.getElementById('1010.1588v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1010.1588v2-abstract-full" style="display: none;"> From the launch of the Fermi Gamma-ray Space Telescope to July 9, 2010, the Gamma-ray Burst Monitor (GBM) has detected 497 probable GRB events. Twenty-two of these satisfy the simultaneous requirements of an estimated burst direction within 52^\circ of the Fermi Large Area Telescope (LAT) boresight and a low energy fluence exceeding 5 $渭$erg/cm^2. Using matched filter techniques, the spatially correlated Fermi/LAT photon data above 100 MeV have been examined for evidence of bursts that have so far evaded detection at these energies. High energy emission is detected with great confidence for one event, GRB 090228A. Since the LAT has significantly better angular resolution than the GBM, real-time application of these methods could open the door to optical identification and richer characterization of a larger fraction of the relatively rare GRBs that include high energy emission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1010.1588v2-abstract-full').style.display = 'none'; document.getElementById('1010.1588v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 October, 2010; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 October, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2010. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">4 pages, 3 figures, 2 tables, accepted for publication in ApJ Letters, minor revisions</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1010.1436">arXiv:1010.1436</a> <span> [<a href="https://arxiv.org/pdf/1010.1436">pdf</a>, <a href="https://arxiv.org/ps/1010.1436">ps</a>, <a href="https://arxiv.org/format/1010.1436">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/726/1/22">10.1088/0004-637X/726/1/22 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Searching for Needles in Haystacks - Looking for GRB gamma-rays with the Fermi/LAT Detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Zheng%2C+W">W. Zheng</a>, <a href="/search/astro-ph?searchtype=author&query=Pandey%2C+S+B">S. B. Pandey</a>, <a href="/search/astro-ph?searchtype=author&query=McKay%2C+T+A">T. A. McKay</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1010.1436v2-abstract-short" style="display: inline;"> Since the launch of the Fermi Gamma-ray Space Telescope on June 11, 2008, 55 gamma-ray bursts (GRBs) have been observed at coordinates that fall within 66^\circ of the Fermi Large Area Telescope (LAT) boresight with precise localizations provided by the NASA Swift mission or other satellites. Imposing selection cuts to exclude low Galactic latitudes and high zenith angles reduces the sample size t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1010.1436v2-abstract-full').style.display = 'inline'; document.getElementById('1010.1436v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1010.1436v2-abstract-full" style="display: none;"> Since the launch of the Fermi Gamma-ray Space Telescope on June 11, 2008, 55 gamma-ray bursts (GRBs) have been observed at coordinates that fall within 66^\circ of the Fermi Large Area Telescope (LAT) boresight with precise localizations provided by the NASA Swift mission or other satellites. Imposing selection cuts to exclude low Galactic latitudes and high zenith angles reduces the sample size to 41. Using matched filter techniques, the Fermi/LAT photon data for these fields have been examined for evidence of bursts that have so far evaded detection at energies above 100 MeV. Following comparisons with similar random background fields, two events, GRB 080905A and GRB 091208B, stand out as excellent candidates for such an identification. After excluding the six bright bursts previously reported by the LAT team, the remaining 35 events exhibit an excess of LAT "diffuse" photons with a statistical significance greater than 2 sigma, independent of the matched filter analysis. After accounting for the total number of photons in the well-localized fields and including estimates of detection efficiency, one concludes that somewhere in the range of 11% to 19% of all GRBs within the LAT field of view illuminate the detector with two or more energetic photons. These are the most stringent estimates of the high energy photon content of GRBs to date. The two new events associated with high energy photon emission have similar ratios of high to low energy fluences as observed previously. This separates them from bursts with similar low energy fluences by a factor of ten, suggesting a distinct class of events rather than a smooth continuum. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1010.1436v2-abstract-full').style.display = 'none'; document.getElementById('1010.1436v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 October, 2010; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 October, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2010. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 4 figures, 2 tables, accepted for publication in ApJ, minor revisions</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1009.0004">arXiv:1009.0004</a> <span> [<a href="https://arxiv.org/pdf/1009.0004">pdf</a>, <a href="https://arxiv.org/ps/1009.0004">ps</a>, <a href="https://arxiv.org/format/1009.0004">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-6256/141/2/36">10.1088/0004-6256/141/2/36 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Monster in the Dark: The Ultraluminous GRB 080607 and its Dusty Environment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Perley%2C+D+A">Daniel A. Perley</a>, <a href="/search/astro-ph?searchtype=author&query=Morgan%2C+A+N">A. N. Morgan</a>, <a href="/search/astro-ph?searchtype=author&query=Updike%2C+A">A. Updike</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+F">F. Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Miller%2C+A+A">A. A. Miller</a>, <a href="/search/astro-ph?searchtype=author&query=Bloom%2C+J+S">J. S. Bloom</a>, <a href="/search/astro-ph?searchtype=author&query=Cenko%2C+S+B">S. B. Cenko</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+W">W. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Filippenko%2C+A+V">A. V. Filippenko</a>, <a href="/search/astro-ph?searchtype=author&query=Prochaska%2C+J+X">J. X. Prochaska</a>, <a href="/search/astro-ph?searchtype=author&query=Kann%2C+D+A">D. A. Kann</a>, <a href="/search/astro-ph?searchtype=author&query=Butler%2C+N+R">N. R. Butler</a>, <a href="/search/astro-ph?searchtype=author&query=Christian%2C+P">P. Christian</a>, <a href="/search/astro-ph?searchtype=author&query=Hartmann%2C+D+H">D. H. Hartmann</a>, <a href="/search/astro-ph?searchtype=author&query=Milne%2C+P">P. Milne</a>, <a href="/search/astro-ph?searchtype=author&query=Rykoff%2C+E+S">E. S. Rykoff</a>, <a href="/search/astro-ph?searchtype=author&query=Rujopakarn%2C+W">W. Rujopakarn</a>, <a href="/search/astro-ph?searchtype=author&query=Wheeler%2C+J+C">J. C. Wheeler</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+G+G">G. G. Williams</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1009.0004v1-abstract-short" style="display: inline;"> We present early-time optical through infrared photometry of the bright gamma-ray burst GRB 080607, starting only 6 s following the initial trigger in the rest frame. Complemented by our previously published spectroscopy, this high-quality photometric dataset allows us to solve for the extinction properties of the redshift 3.036 sightline, giving perhaps the most detailed information on the ultrav… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1009.0004v1-abstract-full').style.display = 'inline'; document.getElementById('1009.0004v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1009.0004v1-abstract-full" style="display: none;"> We present early-time optical through infrared photometry of the bright gamma-ray burst GRB 080607, starting only 6 s following the initial trigger in the rest frame. Complemented by our previously published spectroscopy, this high-quality photometric dataset allows us to solve for the extinction properties of the redshift 3.036 sightline, giving perhaps the most detailed information on the ultraviolet continuum absorption properties of any sightline outside our Local Group to date. The extinction properties are not adequately modeled by any ordinary extinction template (including the average Milky Way, Large Magellanic Cloud, and Small Magellanic Cloud curves), partially because the 2175-Angstrom feature (while present) is weaker by about a factor of two than when seen under similar circumstances locally. However, the spectral energy distribution is exquisitely fitted by the more general Fitzpatrick & Massa (1990) parameterization of Local-Group extinction, putting it in the same family as some peculiar Milky Way extinction curves. After correcting for this (considerable, A_V = 3.3 +/- 0.4 mag) extinction, GRB 080607 is revealed to have been among the most optically luminous events ever observed, comparable to the naked-eye burst GRB 080319B. Its early peak time (t_rest < 6 s) indicates a high initial Lorentz factor (Gamma > 600), while the extreme luminosity may be explained in part by a large circumburst density. Only because of its early high luminosity could the afterglow of GRB 080607 be studied in such detail in spite of the large attenuation and great distance, making this burst an excellent prototype for the understanding of other highly obscured extragalactic objects, and of the class of "dark" GRBs in particular. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1009.0004v1-abstract-full').style.display = 'none'; document.getElementById('1009.0004v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 August, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2010. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to AJ. 15 pages, 6 tables, 9 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1007.0383">arXiv:1007.0383</a> <span> [<a href="https://arxiv.org/pdf/1007.0383">pdf</a>, <a href="https://arxiv.org/ps/1007.0383">ps</a>, <a href="https://arxiv.org/format/1007.0383">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201015324">10.1051/0004-6361/201015324 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Swift/Fermi GRB 080928 from 1 eV to 150 keV </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rossi%2C+A">A. Rossi</a>, <a href="/search/astro-ph?searchtype=author&query=Schulze%2C+S">S. Schulze</a>, <a href="/search/astro-ph?searchtype=author&query=Klose%2C+S">S. Klose</a>, <a href="/search/astro-ph?searchtype=author&query=Kann%2C+D+A">D. A. Kann</a>, <a href="/search/astro-ph?searchtype=author&query=Rau%2C+A">A. Rau</a>, <a href="/search/astro-ph?searchtype=author&query=Krimm%2C+H+A">H. A. Krimm</a>, <a href="/search/astro-ph?searchtype=author&query=J%C3%B3hannesson%2C+G">G. J贸hannesson</a>, <a href="/search/astro-ph?searchtype=author&query=Panaitescu%2C+A">A. Panaitescu</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+F">F. Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrero%2C+P">P. Ferrero</a>, <a href="/search/astro-ph?searchtype=author&query=Kr%C3%BChler%2C+T">T. Kr眉hler</a>, <a href="/search/astro-ph?searchtype=author&query=Greiner%2C+J">J. Greiner</a>, <a href="/search/astro-ph?searchtype=author&query=Schady%2C+P">P. Schady</a>, <a href="/search/astro-ph?searchtype=author&query=Pandey%2C+S+B">S. B. Pandey</a>, <a href="/search/astro-ph?searchtype=author&query=Amati%2C+L">L. Amati</a>, <a href="/search/astro-ph?searchtype=author&query=Afonso%2C+P+M+J">P. M. J. Afonso</a>, <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Arnold%2C+L">L. Arnold</a>, <a href="/search/astro-ph?searchtype=author&query=Clemens%2C+C">C. Clemens</a>, <a href="/search/astro-ph?searchtype=author&query=Filgas%2C+R">R. Filgas</a>, <a href="/search/astro-ph?searchtype=author&query=Hartmann%2C+D+H">D. H. Hartmann</a>, <a href="/search/astro-ph?searchtype=author&query=Yolda%C5%9F%2C+A+K">A. K眉pc眉 Yolda艧</a>, <a href="/search/astro-ph?searchtype=author&query=McBreen%2C+S">S. McBreen</a>, <a href="/search/astro-ph?searchtype=author&query=McKay%2C+T+A">T. A. McKay</a>, <a href="/search/astro-ph?searchtype=author&query=Guelbenzu%2C+A+N">A. Nicuesa Guelbenzu</a> , et al. (6 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1007.0383v4-abstract-short" style="display: inline;"> We present the results of a comprehensive study of the gamma-ray burst 080928 and of its afterglow. GRB 080928 was a long burst detected by Swift/BAT and Fermi/GBM. It is one of the exceptional cases where optical emission had already been detected when the GRB itself was still radiating in the gamma-ray band. For nearly 100 seconds simultaneous optical, X-ray and gamma-ray data provide a coverage… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1007.0383v4-abstract-full').style.display = 'inline'; document.getElementById('1007.0383v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1007.0383v4-abstract-full" style="display: none;"> We present the results of a comprehensive study of the gamma-ray burst 080928 and of its afterglow. GRB 080928 was a long burst detected by Swift/BAT and Fermi/GBM. It is one of the exceptional cases where optical emission had already been detected when the GRB itself was still radiating in the gamma-ray band. For nearly 100 seconds simultaneous optical, X-ray and gamma-ray data provide a coverage of the spectral energy distribution of the transient source from about 1 eV to 150 keV. In particular, we show that the SED during the main prompt emission phase agrees with synchrotron radiation. We constructed the optical/near-infrared light curve and the spectral energy distribution based on Swift/UVOT, ROTSE-IIIa (Australia), and GROND (La Silla) data and compared it to the X-ray light curve retrieved from the Swift/XRT repository. We show that its bumpy shape can be modeled by multiple energy-injections into the forward shock.Furthermore, we investigate whether the temporal and spectral evolution of the tail emission of the first strong flare seen in the early X-ray light curve can be explained by large-angle emission (LAE). We find that a nonstandard LAE model is required to explain the observations. Finally, we report on the results of our search for the GRB host galaxy, for which only a deep upper limit can be provided. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1007.0383v4-abstract-full').style.display = 'none'; document.getElementById('1007.0383v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 March, 2011; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 July, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2010. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">A&A, in press (including revisions according to the language editor), 14 pages, 11 figures, 7 tables; Online Appendix: 4 pages, 1 figure, 4 tables; v4: final journal version to be published soon</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1004.3329">arXiv:1004.3329</a> <span> [<a href="https://arxiv.org/pdf/1004.3329">pdf</a>, <a href="https://arxiv.org/ps/1004.3329">ps</a>, <a href="https://arxiv.org/format/1004.3329">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/715/2/1338">10.1088/0004-637X/715/2/1338 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Exceptionally Luminous Type Ia Supernova 2007if </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+F">F. Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Quimby%2C+R+M">R. M. Quimby</a>, <a href="/search/astro-ph?searchtype=author&query=Wheeler%2C+J+C">J. C. Wheeler</a>, <a href="/search/astro-ph?searchtype=author&query=Vinko%2C+J">J. Vinko</a>, <a href="/search/astro-ph?searchtype=author&query=Chatzopoulos%2C+E">E. Chatzopoulos</a>, <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Kulkarni%2C+S">S. Kulkarni</a>, <a href="/search/astro-ph?searchtype=author&query=Miller%2C+J+M">J. M. Miller</a>, <a href="/search/astro-ph?searchtype=author&query=McKay%2C+T+A">T. A. McKay</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1004.3329v2-abstract-short" style="display: inline;"> SN 2007if was the third over-luminous SN Ia detected after 2003fg and 2006gz. We present the photometric and spectroscopic observations of the supernova and its host by ROTSE-III, HET and Keck. From the H_alpha line identified in the host spectra, we determine a redshift of 0.0736. At this distance, the supernova reached an absolute magnitude of -20.4, brighter than any other SNe Ia ever observed.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1004.3329v2-abstract-full').style.display = 'inline'; document.getElementById('1004.3329v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1004.3329v2-abstract-full" style="display: none;"> SN 2007if was the third over-luminous SN Ia detected after 2003fg and 2006gz. We present the photometric and spectroscopic observations of the supernova and its host by ROTSE-III, HET and Keck. From the H_alpha line identified in the host spectra, we determine a redshift of 0.0736. At this distance, the supernova reached an absolute magnitude of -20.4, brighter than any other SNe Ia ever observed. If the source of luminosity is radioactive decay, a large amount of radioactive nickel (~1.5 solar masses) is required to power the peak luminosity, more than can be produced realistically in a Chandrasekhar mass progenitor. Low expansion velocity, similar to that of 2003fg, is also measured around the maximum light. The observations may suggest that SN 2007if was from a massive white dwarf progenitor, plausibly exploding with mass well beyond 1.4 solar masses. Alternatively, we investigate circumstellar interaction that may contribute to the excess luminosity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1004.3329v2-abstract-full').style.display = 'none'; document.getElementById('1004.3329v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 April, 2010; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 April, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2010. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">7 pages, 7 figures, accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1002.0581">arXiv:1002.0581</a> <span> [<a href="https://arxiv.org/pdf/1002.0581">pdf</a>, <a href="https://arxiv.org/ps/1002.0581">ps</a>, <a href="https://arxiv.org/format/1002.0581">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/711/2/870">10.1088/0004-637X/711/2/870 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> GRB 081008: from burst to afterglow and the transition phase in between </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+F">F. Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Schady%2C+P">P. Schady</a>, <a href="/search/astro-ph?searchtype=author&query=Racusin%2C+J+L">J. L. Racusin</a>, <a href="/search/astro-ph?searchtype=author&query=Willingale%2C+R">R. Willingale</a>, <a href="/search/astro-ph?searchtype=author&query=Kruhler%2C+T">T. Kruhler</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Brien%2C+P+T">P. T. O'Brien</a>, <a href="/search/astro-ph?searchtype=author&query=Greiner%2C+J">J. Greiner</a>, <a href="/search/astro-ph?searchtype=author&query=Oates%2C+S+R">S. R. Oates</a>, <a href="/search/astro-ph?searchtype=author&query=Rykoff%2C+E+S">E. S. Rykoff</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Ashley%2C+M+C+B">M. C. B. Ashley</a>, <a href="/search/astro-ph?searchtype=author&query=Barthelmy%2C+S+D">S. D. Barthelmy</a>, <a href="/search/astro-ph?searchtype=author&query=Filgas%2C+R">R. Filgas</a>, <a href="/search/astro-ph?searchtype=author&query=Flewelling%2C+H+A">H. A. Flewelling</a>, <a href="/search/astro-ph?searchtype=author&query=Gehrels%2C+N">N. Gehrels</a>, <a href="/search/astro-ph?searchtype=author&query=Gogus%2C+E">E. Gogus</a>, <a href="/search/astro-ph?searchtype=author&query=Guver%2C+T">T. Guver</a>, <a href="/search/astro-ph?searchtype=author&query=Horns%2C+D">D. Horns</a>, <a href="/search/astro-ph?searchtype=author&query=Kiziloglu%2C+U">U. Kiziloglu</a>, <a href="/search/astro-ph?searchtype=author&query=Krimm%2C+H+A">H. A. Krimm</a>, <a href="/search/astro-ph?searchtype=author&query=McKay%2C+T+A">T. A. McKay</a>, <a href="/search/astro-ph?searchtype=author&query=Ozel%2C+M+E">M. E. Ozel</a>, <a href="/search/astro-ph?searchtype=author&query=Pandey%2C+S+B">S. B. Pandey</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+A">A. Phillips</a> , et al. (8 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1002.0581v1-abstract-short" style="display: inline;"> We present a multi-wavelength study of GRB 081008, at redshift 1.967, by Swift, ROTSE-III and GROND. Compared to other Swift GRBs, GRB 081008 has a typical gamma-ray isotropic equivalent energy output (10^53 erg) during the prompt phase, and displayed two temporally separated clusters of pulses. The early X-ray emission seen by the Swift/XRT was dominated by the softening tail of the prompt emis… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1002.0581v1-abstract-full').style.display = 'inline'; document.getElementById('1002.0581v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1002.0581v1-abstract-full" style="display: none;"> We present a multi-wavelength study of GRB 081008, at redshift 1.967, by Swift, ROTSE-III and GROND. Compared to other Swift GRBs, GRB 081008 has a typical gamma-ray isotropic equivalent energy output (10^53 erg) during the prompt phase, and displayed two temporally separated clusters of pulses. The early X-ray emission seen by the Swift/XRT was dominated by the softening tail of the prompt emission, producing multiple flares during and after the Swift/BAT detections. Optical observations that started shortly after the first active phase of gamma-ray emission showed two consecutive peaks. We interpret the first optical peak as the onset of the afterglow associated with the early burst activities. A second optical peak, coincident with the later gamma-ray pulses, imposes a small modification to the otherwise smooth lightcurve and thus suggests a minimal contribution from a probable internal component. We suggest the early optical variability may be from continuous energy injection into the forward shock front by later shells producing the second epoch of burst activities. These early observations thus provide a potential probe for the transition from prompt to the afterglow phase. The later lightcurve of GRB 081008 displays a smooth steepening in all optical bands and X-ray. The temporal break is consistent with being achromatic at the observed wavelengths. Our broad energy coverage shortly after the break constrains a spectral break within optical. However, the evolution of the break frequency is not observed. We discuss the plausible interpretations of this behavior. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1002.0581v1-abstract-full').style.display = 'none'; document.getElementById('1002.0581v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 February, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2010. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 4 figures, accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0912.3026">arXiv:0912.3026</a> <span> [<a href="https://arxiv.org/pdf/0912.3026">pdf</a>, <a href="https://arxiv.org/ps/0912.3026">ps</a>, <a href="https://arxiv.org/format/0912.3026">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Prompt optical observations of Fermi-LAT bursts and GRB 090902B </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pandey%2C+S+B">S. B. Pandey</a>, <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">Carl W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Zheng%2C+W">W. Zheng</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+F">F. Yuan</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="0912.3026v1-abstract-short" style="display: inline;"> Observations of high energy emission from gamma-ray bursts (GRBs) constrain the extreme physical conditions associated with these energetic cosmic explosions. The Large Area Telescope (LAT) onboard the Fermi Gamma-ray Space Telescope, a pair conversion telescope, observes energetic quanta from 30 MeV to > 300 GeV. Synergy of the LAT with the Gamma-ray Burst Monitor (GBM) enlarges the energy cove… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0912.3026v1-abstract-full').style.display = 'inline'; document.getElementById('0912.3026v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0912.3026v1-abstract-full" style="display: none;"> Observations of high energy emission from gamma-ray bursts (GRBs) constrain the extreme physical conditions associated with these energetic cosmic explosions. The Large Area Telescope (LAT) onboard the Fermi Gamma-ray Space Telescope, a pair conversion telescope, observes energetic quanta from 30 MeV to > 300 GeV. Synergy of the LAT with the Gamma-ray Burst Monitor (GBM) enlarges the energy coverage to ~ 7.5 decades, very useful for studying the GRB emission itself. Prompt optical observations and their possible correlations with photon emission at LAT energies help our understanding of the physical mechanisms behind these events. The prompt response times and large fields of of the ROTSE-III telescopes make afterglow observations possible for Fermi bursts with ~ 1 degree localized errors. As an example, GRB 090902B, was observed starting ~ 4803 s after the burst. This is the earliest ground-based optical detection ever made for long-duration bursts sensed by the LAT. The ROTSE detection classifies the optical afterglow of GRB 090902B as one of the brightest. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0912.3026v1-abstract-full').style.display = 'none'; document.getElementById('0912.3026v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 December, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2009. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">4 pages, 4 figures, 2009 Fermi Symposium, eConf Proceedings C091122</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0904.0261">arXiv:0904.0261</a> <span> [<a href="https://arxiv.org/pdf/0904.0261">pdf</a>, <a href="https://arxiv.org/ps/0904.0261">ps</a>, <a href="https://arxiv.org/format/0904.0261">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/702/1/489">10.1088/0004-637X/702/1/489 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Looking Into the Fireball: ROTSE-III and Swift Observations of Early GRB Afterglows </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rykoff%2C+E+S">E. S. Rykoff</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Ashley%2C+M+C+B">M. C. B. Ashley</a>, <a href="/search/astro-ph?searchtype=author&query=Barthelmy%2C+S+D">S. D. Barthelmy</a>, <a href="/search/astro-ph?searchtype=author&query=Flewelling%2C+H+A">H. A. Flewelling</a>, <a href="/search/astro-ph?searchtype=author&query=Gehrels%2C+N">N. Gehrels</a>, <a href="/search/astro-ph?searchtype=author&query=Gogus%2C+E">E. Gogus</a>, <a href="/search/astro-ph?searchtype=author&query=Guver%2C+T">T. Guver</a>, <a href="/search/astro-ph?searchtype=author&query=Kiziloglu%2C+U">U. Kiziloglu</a>, <a href="/search/astro-ph?searchtype=author&query=Krimm%2C+H+A">H. A. Krimm</a>, <a href="/search/astro-ph?searchtype=author&query=McKay%2C+T+A">T. A. McKay</a>, <a href="/search/astro-ph?searchtype=author&query=Ozel%2C+M">M. Ozel</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+A">A. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Quimby%2C+R+M">R. M. Quimby</a>, <a href="/search/astro-ph?searchtype=author&query=Rowell%2C+G">G. Rowell</a>, <a href="/search/astro-ph?searchtype=author&query=Rujopakarn%2C+W">W. Rujopakarn</a>, <a href="/search/astro-ph?searchtype=author&query=Schaefer%2C+B+E">B. E. Schaefer</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+D+A">D. A. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Vestrand%2C+W+T">W. T. Vestrand</a>, <a href="/search/astro-ph?searchtype=author&query=Wheeler%2C+J+C">J. C. Wheeler</a>, <a href="/search/astro-ph?searchtype=author&query=Wren%2C+J">J. Wren</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+F">F. Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Yost%2C+S+A">S. A. Yost</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="0904.0261v1-abstract-short" style="display: inline;"> We report on a complete set of early optical afterglows of gamma-ray bursts (GRBs) obtained with the ROTSE-III telescope network from March 2005 through June 2007. This set is comprised of 12 afterglows with early optical and Swift/XRT observations, with a median ROTSE-III response time of 45 s after the start of gamma-ray emission (8 s after the GCN notice time). These afterglows span four orde… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0904.0261v1-abstract-full').style.display = 'inline'; document.getElementById('0904.0261v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0904.0261v1-abstract-full" style="display: none;"> We report on a complete set of early optical afterglows of gamma-ray bursts (GRBs) obtained with the ROTSE-III telescope network from March 2005 through June 2007. This set is comprised of 12 afterglows with early optical and Swift/XRT observations, with a median ROTSE-III response time of 45 s after the start of gamma-ray emission (8 s after the GCN notice time). These afterglows span four orders of magnitude in optical luminosity, and the contemporaneous X-ray detections allow multi-wavelength spectral analysis. Excluding X-ray flares, the broadband synchrotron spectra show that the optical and X-ray emission originate in a common region, consistent with predictions of the external forward shock in the fireball model. However, the fireball model is inadequate to predict the temporal decay indices of the early afterglows, even after accounting for possible long-duration continuous energy injection. We find that the optical afterglow is a clean tracer of the forward shock, and we use the peak time of the forward shock to estimate the initial bulk Lorentz factor of the GRB outflow, and find 100<Gamma_0<1000, consistent with expectations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0904.0261v1-abstract-full').style.display = 'none'; document.getElementById('0904.0261v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 April, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2009. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">31 pages, 5 figures, submitted to ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.702:489-505,2009 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0806.1182">arXiv:0806.1182</a> <span> [<a href="https://arxiv.org/pdf/0806.1182">pdf</a>, <a href="https://arxiv.org/ps/0806.1182">ps</a>, <a href="https://arxiv.org/format/0806.1182">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/200810340">10.1051/0004-6361/200810340 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Photometry and spectroscopy of GRB 060526: A detailed study of the afterglow and host galaxy of a z=3.2 gamma-ray burst </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Th%C3%B6ne%2C+C+C">C. C. Th枚ne</a>, <a href="/search/astro-ph?searchtype=author&query=Kann%2C+D+A">D. A. Kann</a>, <a href="/search/astro-ph?searchtype=author&query=J%C3%B3hannesson%2C+G">G. J贸hannesson</a>, <a href="/search/astro-ph?searchtype=author&query=Selj%2C+J+H">J. H. Selj</a>, <a href="/search/astro-ph?searchtype=author&query=Jaunsen%2C+A+O">A. O. Jaunsen</a>, <a href="/search/astro-ph?searchtype=author&query=Fynbo%2C+J+P+U">J. P. U. Fynbo</a>, <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Baliyan%2C+K+S">K. S. Baliyan</a>, <a href="/search/astro-ph?searchtype=author&query=Bartolini%2C+C">C. Bartolini</a>, <a href="/search/astro-ph?searchtype=author&query=Bikmaev%2C+I+F">I. F. Bikmaev</a>, <a href="/search/astro-ph?searchtype=author&query=Bloom%2C+J+S">J. S. Bloom</a>, <a href="/search/astro-ph?searchtype=author&query=Burenin%2C+R+A">R. A. Burenin</a>, <a href="/search/astro-ph?searchtype=author&query=Cobb%2C+B+E">B. E. Cobb</a>, <a href="/search/astro-ph?searchtype=author&query=Covino%2C+S">S. Covino</a>, <a href="/search/astro-ph?searchtype=author&query=Curran%2C+P+A">P. A. Curran</a>, <a href="/search/astro-ph?searchtype=author&query=Dahle%2C+H">H. Dahle</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrero%2C+A">A. Ferrero</a>, <a href="/search/astro-ph?searchtype=author&query=Foley%2C+S">S. Foley</a>, <a href="/search/astro-ph?searchtype=author&query=French%2C+J">J. French</a>, <a href="/search/astro-ph?searchtype=author&query=Fruchter%2C+A+S">A. S. Fruchter</a>, <a href="/search/astro-ph?searchtype=author&query=Ganesh%2C+S">S. Ganesh</a>, <a href="/search/astro-ph?searchtype=author&query=Graham%2C+J+F">J. F. Graham</a>, <a href="/search/astro-ph?searchtype=author&query=Greco%2C+G">G. Greco</a>, <a href="/search/astro-ph?searchtype=author&query=Guarnieri%2C+A">A. Guarnieri</a>, <a href="/search/astro-ph?searchtype=author&query=Hanlon%2C+L">L. Hanlon</a> , et al. (36 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="0806.1182v3-abstract-short" style="display: inline;"> Aims: With this paper we want to investigate the highly variable afterglow light curve and environment of gamma-ray burst (GRB) 060526 at $z=3.221$. Methods: We present one of the largest photometric datasets ever obtained for a GRB afterglow, consisting of multi-color photometric data from the ultraviolet to the near infrared. The data set contains 412 data points in total to which we add additio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0806.1182v3-abstract-full').style.display = 'inline'; document.getElementById('0806.1182v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0806.1182v3-abstract-full" style="display: none;"> Aims: With this paper we want to investigate the highly variable afterglow light curve and environment of gamma-ray burst (GRB) 060526 at $z=3.221$. Methods: We present one of the largest photometric datasets ever obtained for a GRB afterglow, consisting of multi-color photometric data from the ultraviolet to the near infrared. The data set contains 412 data points in total to which we add additional data from the literature. Furthermore, we present low-resolution high signal-to-noise spectra of the afterglow. The afterglow light curve is modeled with both an analytical model using broken power law fits and with a broad-band numerical model which includes energy injections. The absorption lines detected in the spectra are used to derive column densities using a multi-ion single-component curve-of-growth analysis from which we derive the metallicity of the host of GRB 060526. Results: The temporal behaviour of the afterglow follows a double broken power law with breaks at $t=0.090\pm0.005$ and $t=2.401\pm0.061$ days. It shows deviations from the smooth set of power laws that can be modeled by additional energy injections from the central engine, although some significant microvariability remains. The broadband spectral-energy distribution of the afterglow shows no significant extinction along the line of sight. The metallicity derived from \ion{S}{II} and \ion{Fe}{II} of [S/H] = --0.57 $\pm$0.25 and [Fe/H] = --1.09$\pm$0.24 is relatively high for a galaxy at that redshift but comparable to the metallicity of other GRB hosts at similar redshifts. At the position of the afterglow, no host is detected to F775W(AB) = 28.5 mag with the HST, implying an absolute magnitude of the host M(1500 脜)$>$--18.3 mag which is fainter than most long-duration hosts, although the GRB may be associated with a faint galaxy at a distance of 11 kpc. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0806.1182v3-abstract-full').style.display = 'none'; document.getElementById('0806.1182v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 July, 2010; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 June, 2008; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2008. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 8 figures, A&A, in press, three additional authors, additional minor changes after second referee report</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astron.Astrophys.523:A70,2010 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0801.0336">arXiv:0801.0336</a> <span> [<a href="https://arxiv.org/pdf/0801.0336">pdf</a>, <a href="https://arxiv.org/ps/0801.0336">ps</a>, <a href="https://arxiv.org/format/0801.0336">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/529040">10.1086/529040 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Astronomical Image Subtraction by Cross-Convolution </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+F">Fang Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">Carl W. Akerlof</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="0801.0336v1-abstract-short" style="display: inline;"> In recent years, there has been a proliferation of wide-field sky surveys to search for a variety of transient objects. Using relatively short focal lengths, the optics of these systems produce undersampled stellar images often marred by a variety of aberrations. As participants in such activities, we have developed a new algorithm for image subtraction that no longer requires high quality refer… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0801.0336v1-abstract-full').style.display = 'inline'; document.getElementById('0801.0336v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0801.0336v1-abstract-full" style="display: none;"> In recent years, there has been a proliferation of wide-field sky surveys to search for a variety of transient objects. Using relatively short focal lengths, the optics of these systems produce undersampled stellar images often marred by a variety of aberrations. As participants in such activities, we have developed a new algorithm for image subtraction that no longer requires high quality reference images for comparison. The computational efficiency is comparable with similar procedures currently in use. The general technique is cross-convolution: two convolution kernels are generated to make a test image and a reference image separately transform to match as closely as possible. In analogy to the optimization technique for generating smoothing splines, the inclusion of an RMS width penalty term constrains the diffusion of stellar images. In addition, by evaluating the convolution kernels on uniformly spaced subimages across the total area, these routines can accomodate point spread functions that vary considerably across the focal plane. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0801.0336v1-abstract-full').style.display = 'none'; document.getElementById('0801.0336v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 January, 2008; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2008. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">6 pages including 2 figures, accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0709.0962">arXiv:0709.0962</a> <span> [<a href="https://arxiv.org/pdf/0709.0962">pdf</a>, <a href="https://arxiv.org/ps/0709.0962">ps</a>, <a href="https://arxiv.org/format/0709.0962">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/523081">10.1086/523081 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An Estimation of the Gamma-Ray Burst Afterglow Apparent Optical Brightness Distribution Function </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">Carl W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Swan%2C+H+F">Heather F. Swan</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="0709.0962v1-abstract-short" style="display: inline;"> By using recent publicly available observational data obtained in conjunction with the NASA Swift gamma-ray burst mission and a novel data analysis technique, we have been able to make some rough estimates of the GRB afterglow apparent optical brightness distribution function. The results suggest that 71% of all burst afterglows have optical magnitudes with mR < 22.1 at 1000 seconds after the bu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0709.0962v1-abstract-full').style.display = 'inline'; document.getElementById('0709.0962v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0709.0962v1-abstract-full" style="display: none;"> By using recent publicly available observational data obtained in conjunction with the NASA Swift gamma-ray burst mission and a novel data analysis technique, we have been able to make some rough estimates of the GRB afterglow apparent optical brightness distribution function. The results suggest that 71% of all burst afterglows have optical magnitudes with mR < 22.1 at 1000 seconds after the burst onset, the dimmest detected object in the data sample. There is a strong indication that the apparent optical magnitude distribution function peaks at mR ~ 19.5. Such estimates may prove useful in guiding future plans to improve GRB counterpart observation programs. The employed numerical techniques might find application in a variety of other data analysis problems in which the intrinsic distributions must be inferred from a heterogeneous sample. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0709.0962v1-abstract-full').style.display = 'none'; document.getElementById('0709.0962v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 September, 2007; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2007. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages including 2 tables and 7 figures, accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0709.0302">arXiv:0709.0302</a> <span> [<a href="https://arxiv.org/pdf/0709.0302">pdf</a>, <a href="https://arxiv.org/ps/0709.0302">ps</a>, <a href="https://arxiv.org/format/0709.0302">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/522862">10.1086/522862 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> SN 2005ap: A Most Brilliant Explosion </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Quimby%2C+R+M">Robert M. Quimby</a>, <a href="/search/astro-ph?searchtype=author&query=Aldering%2C+G">Greg Aldering</a>, <a href="/search/astro-ph?searchtype=author&query=Wheeler%2C+J+C">J. Craig Wheeler</a>, <a href="/search/astro-ph?searchtype=author&query=H%C3%B6flich%2C+P">Peter H枚flich</a>, <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">Carl W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Rykoff%2C+E+S">Eli S. Rykoff</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="0709.0302v1-abstract-short" style="display: inline;"> We present unfiltered photometric observations with ROTSE-III and optical spectroscopic follow-up with the HET and Keck of the most luminous supernova yet identified, SN 2005ap. The spectra taken about 3 days before and 6 days after maximum light show narrow emission lines (likely originating in the dwarf host) and absorption lines at a redshift of z=0.2832, which puts the peak unfiltered magnit… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0709.0302v1-abstract-full').style.display = 'inline'; document.getElementById('0709.0302v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0709.0302v1-abstract-full" style="display: none;"> We present unfiltered photometric observations with ROTSE-III and optical spectroscopic follow-up with the HET and Keck of the most luminous supernova yet identified, SN 2005ap. The spectra taken about 3 days before and 6 days after maximum light show narrow emission lines (likely originating in the dwarf host) and absorption lines at a redshift of z=0.2832, which puts the peak unfiltered magnitude at -22.7 +/- 0.1 absolute. Broad P-Cygni features corresponding to H-alpha, CIII, NIII, and OIII, are further detected with a photospheric velocity of ~20,000 km/s. Unlike other highly luminous supernovae such as 2006gy and 2006tf that show slow photometric evolution, the light curve of SN 2005ap indicates a 1-3 week rise to peak followed by a relatively rapid decay. The spectra also lack the distinct emission peaks from moderately broadened (FWHM ~ 2,000 km/s) Balmer lines seen in SN 2006gy and SN 2006tf. We briefly discuss the origin of the extraordinary luminosity from a strong interaction as may be expected from a pair instability eruption or a GRB-like engine encased in a H/He envelope. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0709.0302v1-abstract-full').style.display = 'none'; document.getElementById('0709.0302v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 September, 2007; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2007. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">ApJ Letters Accepted; 4 pages</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0707.3132">arXiv:0707.3132</a> <span> [<a href="https://arxiv.org/pdf/0707.3132">pdf</a>, <a href="https://arxiv.org/ps/0707.3132">ps</a>, <a href="https://arxiv.org/format/0707.3132">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/521668">10.1086/521668 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Dark Side of ROTSE-III Prompt GRB Observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Yost%2C+S+A">S. A. Yost</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Ashley%2C+M+C+B">M. C. B. Ashley</a>, <a href="/search/astro-ph?searchtype=author&query=Barthelmy%2C+S">S. Barthelmy</a>, <a href="/search/astro-ph?searchtype=author&query=Gehrels%2C+N">N. Gehrels</a>, <a href="/search/astro-ph?searchtype=author&query=Gogus%2C+E">E. Gogus</a>, <a href="/search/astro-ph?searchtype=author&query=Guver%2C+T">T. Guver</a>, <a href="/search/astro-ph?searchtype=author&query=Horns%2C+D">D. Horns</a>, <a href="/search/astro-ph?searchtype=author&query=Kiziloglu%2C+U">U. Kiziloglu</a>, <a href="/search/astro-ph?searchtype=author&query=Krimm%2C+H+A">H. A. Krimm</a>, <a href="/search/astro-ph?searchtype=author&query=McKay%2C+T+A">T. A. McKay</a>, <a href="/search/astro-ph?searchtype=author&query=Ozel%2C+M">M. Ozel</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+A">A. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Quimby%2C+R+M">R. M. Quimby</a>, <a href="/search/astro-ph?searchtype=author&query=Rowell%2C+G">G. Rowell</a>, <a href="/search/astro-ph?searchtype=author&query=Rujopakarn%2C+W">W. Rujopakarn</a>, <a href="/search/astro-ph?searchtype=author&query=Rykoff%2C+E+S">E. S. Rykoff</a>, <a href="/search/astro-ph?searchtype=author&query=Schaefer%2C+B+E">B. E. Schaefer</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+D+A">D. A. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Swan%2C+H+F">H. F. Swan</a>, <a href="/search/astro-ph?searchtype=author&query=Vestrand%2C+W+T">W. T. Vestrand</a>, <a href="/search/astro-ph?searchtype=author&query=Wheeler%2C+J+C">J. C. Wheeler</a>, <a href="/search/astro-ph?searchtype=author&query=Wren%2C+J">J. Wren</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+F">F. Yuan</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="0707.3132v1-abstract-short" style="display: inline;"> We present several cases of optical observations during gamma-ray bursts (GRBs) which resulted in prompt limits but no detection of optical emission. These limits constrain the prompt optical flux densities and the optical brightness relative to the gamma-ray emission. The derived constraints fall within the range of properties observed in GRBs with prompt optical detections, though at the faint… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0707.3132v1-abstract-full').style.display = 'inline'; document.getElementById('0707.3132v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0707.3132v1-abstract-full" style="display: none;"> We present several cases of optical observations during gamma-ray bursts (GRBs) which resulted in prompt limits but no detection of optical emission. These limits constrain the prompt optical flux densities and the optical brightness relative to the gamma-ray emission. The derived constraints fall within the range of properties observed in GRBs with prompt optical detections, though at the faint end of optical/gamma flux ratios. The presently accessible prompt optical limits do not require a different set of intrinsic or environmental GRB properties, relative to the events with prompt optical detections. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0707.3132v1-abstract-full').style.display = 'none'; document.getElementById('0707.3132v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 July, 2007; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2007. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">ApJ accepted. 20 pages in draft manuscript form, which includes 6 pages of tables and 2 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0705.3478">arXiv:0705.3478</a> <span> [<a href="https://arxiv.org/pdf/0705.3478">pdf</a>, <a href="https://arxiv.org/ps/0705.3478">ps</a>, <a href="https://arxiv.org/format/0705.3478">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/520532">10.1086/520532 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> SN 2006bp: Probing the Shock Breakout of a Type II-P Supernova </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Quimby%2C+R+M">Robert M. Quimby</a>, <a href="/search/astro-ph?searchtype=author&query=Wheeler%2C+J+C">J. Craig Wheeler</a>, <a href="/search/astro-ph?searchtype=author&query=H%C3%B6flich%2C+P">Peter H枚flich</a>, <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">Carl W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+P+J">Peter J. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Rykoff%2C+E+S">Eli S. Rykoff</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="0705.3478v1-abstract-short" style="display: inline;"> HET optical spectroscopy and unfiltered ROTSE-III photometry spanning the first 11 months since explosion of the Type II-P SN 2006bp are presented. Flux limits from the days before discovery combined with the initial rapid brightening suggest the supernova was first detected just hours after shock breakout. Optical spectra obtained about 2 days after breakout exhibit narrow emission lines corres… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0705.3478v1-abstract-full').style.display = 'inline'; document.getElementById('0705.3478v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0705.3478v1-abstract-full" style="display: none;"> HET optical spectroscopy and unfiltered ROTSE-III photometry spanning the first 11 months since explosion of the Type II-P SN 2006bp are presented. Flux limits from the days before discovery combined with the initial rapid brightening suggest the supernova was first detected just hours after shock breakout. Optical spectra obtained about 2 days after breakout exhibit narrow emission lines corresponding to HeII 4200, HeII 4686, and CIV 5805 in the rest frame, and these features persist in a second observation obtained 5 hours later; however, these emission lines are not detected the following night nor in subsequent observations. We suggest that these lines emanate from material close to the explosion site, possibly in the outer layers of the progenitor that have been ionized by the high energy photons released at shock breakout. A P-Cygni profile is observed around 4450 A in the +2 and +3 day spectra. Previous studies have attributed this feature to high velocity H-beta, but we discuss the possibility that this profile is instead due to HeII 4687. Further HET observations (14 nights in total) covering the spectral evolution across the photometric plateau up to 73 days after breakout and during the nebular phase around day +340 are presented, and expansion velocities are derived for key features. The measured decay slope for the unfiltered light curve is 0.0073 +/- 0.0004 mag/day between days +121 and +335, which is significantly slower than the decay of rate 56Co. We combine our HET measurements with published X-ray, UV, and optical data to obtain a quasi-bolometric light curve through day +60. We see a slow cooling over the first 25 days, but no sign of an early sharp peak; any such feature from the shock breakout must have lasted less than ~1 day.[ABRIDGED] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0705.3478v1-abstract-full').style.display = 'none'; document.getElementById('0705.3478v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 May, 2007; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2007. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">ApJ accepted, 43 pages</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.666:1093-1107,2007 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0702295">arXiv:astro-ph/0702295</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0702295">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> </div> <p class="title is-5 mathjax"> Statistical Estimates of Coordinate Error Circles for LAT-detected GRBs </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">Carl W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+F">Fang Yuan</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0702295v2-abstract-short" style="display: inline;"> The GLAST mission to be launched in November 2007 will provide unique information about high energy photon fluxes from gamma-ray bursts. These data will be most useful when combined with multiwavelength observations that provide more complete characterizations of such events. To assist this process, we have estimated the GLAST Large Area Telescope (LAT) angular resolution for the coordinates of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0702295v2-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0702295v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0702295v2-abstract-full" style="display: none;"> The GLAST mission to be launched in November 2007 will provide unique information about high energy photon fluxes from gamma-ray bursts. These data will be most useful when combined with multiwavelength observations that provide more complete characterizations of such events. To assist this process, we have estimated the GLAST Large Area Telescope (LAT) angular resolution for the coordinates of ensembles of photons from GRBs as a function of burst spectral index and fluence. This information may be useful in guiding the development of more effective GRB optical afterglow observation programs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0702295v2-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0702295v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 August, 2007; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 February, 2007; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2007. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">4 pages, 8 figures, poster paper presented at the First GLAST Symposium, February 5-8, 2007, two typos corrected</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0611414">arXiv:astro-ph/0611414</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0611414">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0611414">ps</a>, <a href="https://arxiv.org/format/astro-ph/0611414">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/510896">10.1086/510896 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Exploring Broadband GRB Behavior During gamma-ray Emission </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Yost%2C+S+A">S. A. Yost</a>, <a href="/search/astro-ph?searchtype=author&query=Swan%2C+H+F">H. F. Swan</a>, <a href="/search/astro-ph?searchtype=author&query=Rykoff%2C+E+S">E. S. Rykoff</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Alday%2C+A">A. Alday</a>, <a href="/search/astro-ph?searchtype=author&query=Ashley%2C+M+C+B">M. C. B. Ashley</a>, <a href="/search/astro-ph?searchtype=author&query=Barthelmy%2C+S">S. Barthelmy</a>, <a href="/search/astro-ph?searchtype=author&query=Burrows%2C+D">D. Burrows</a>, <a href="/search/astro-ph?searchtype=author&query=Depoy%2C+D+L">D. L. Depoy</a>, <a href="/search/astro-ph?searchtype=author&query=Dufour%2C+R+J">R. J. Dufour</a>, <a href="/search/astro-ph?searchtype=author&query=Eastman%2C+J+D">J. D. Eastman</a>, <a href="/search/astro-ph?searchtype=author&query=Forgey%2C+R+D">R. D. Forgey</a>, <a href="/search/astro-ph?searchtype=author&query=Gehrels%2C+N">N. Gehrels</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%B6%C4%9F%C3%BC%C5%9F%2C+E">E. G枚臒眉艧</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%BCver%2C+T">T. G眉ver</a>, <a href="/search/astro-ph?searchtype=author&query=Halpern%2C+J+P">J. P. Halpern</a>, <a href="/search/astro-ph?searchtype=author&query=Hardin%2C+L+C">L. C. Hardin</a>, <a href="/search/astro-ph?searchtype=author&query=Horns%2C+D">D. Horns</a>, <a href="/search/astro-ph?searchtype=author&query=K%C4%B1z%C4%B1lo%C7%A7lu%2C+U">U. K谋z谋lo千lu</a>, <a href="/search/astro-ph?searchtype=author&query=Krimm%2C+H+A">H. A. Krimm</a>, <a href="/search/astro-ph?searchtype=author&query=Lepine%2C+S">S. Lepine</a>, <a href="/search/astro-ph?searchtype=author&query=Liang%2C+E+P">E. P. Liang</a>, <a href="/search/astro-ph?searchtype=author&query=Marshall%2C+J+L">J. L. Marshall</a>, <a href="/search/astro-ph?searchtype=author&query=McKay%2C+T+A">T. A. McKay</a> , et al. (22 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0611414v1-abstract-short" style="display: inline;"> The robotic ROTSE-III telescope network detected prompt optical emission contemporaneous with the gamma-ray emission of Swift events GRB051109A and GRB051111. Both datasets have continuous coverage at high signal-to-noise levels from the prompt phase onwards, thus the early observations are readily compared to the Swift XRT and BAT high energy detections. In both cases, the optical afterglow is… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0611414v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0611414v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0611414v1-abstract-full" style="display: none;"> The robotic ROTSE-III telescope network detected prompt optical emission contemporaneous with the gamma-ray emission of Swift events GRB051109A and GRB051111. Both datasets have continuous coverage at high signal-to-noise levels from the prompt phase onwards, thus the early observations are readily compared to the Swift XRT and BAT high energy detections. In both cases, the optical afterglow is established, declining steadily during the prompt emission. For GRB051111, there is evidence of an excess optical component during the prompt emission. The component is consistent with the flux spectrally extrapolated from the gamma-rays, using the gamma-ray spectral index. A compilation of spectral information from previous prompt detections shows that such a component is unusual. The existence of two prompt optical components - one connected to the high-energy emission, the other to separate afterglow flux, as indicated in GRB051111 - is not compatible with a simple ``external-external'' shock model for the GRB and its afterglow. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0611414v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0611414v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 November, 2006; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2006. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">ApJ accepted. 32 pages (in preprint form), 5 tables, 5 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.657:925-941,2007 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0601350">arXiv:astro-ph/0601350</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0601350">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0601350">ps</a>, <a href="https://arxiv.org/format/astro-ph/0601350">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/501007">10.1086/501007 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Anomalous Early Afterglow of GRB 050801 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rykoff%2C+E+S">E. S. Rykoff</a>, <a href="/search/astro-ph?searchtype=author&query=Mangano%2C+V">V. Mangano</a>, <a href="/search/astro-ph?searchtype=author&query=Yost%2C+S+A">S. A. Yost</a>, <a href="/search/astro-ph?searchtype=author&query=Sari%2C+R">R. Sari</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Ashley%2C+M+C+B">M. C. B. Ashley</a>, <a href="/search/astro-ph?searchtype=author&query=Barthelmy%2C+S+D">S. D. Barthelmy</a>, <a href="/search/astro-ph?searchtype=author&query=Burrows%2C+D+N">D. N. Burrows</a>, <a href="/search/astro-ph?searchtype=author&query=Gehrels%2C+N">N. Gehrels</a>, <a href="/search/astro-ph?searchtype=author&query=Gogus%2C+E">E. Gogus</a>, <a href="/search/astro-ph?searchtype=author&query=Horns%2C+D">D. Horns</a>, <a href="/search/astro-ph?searchtype=author&query=Kiziloglu%2C+U">U. Kiziloglu</a>, <a href="/search/astro-ph?searchtype=author&query=Krimm%2C+H+A">H. A. Krimm</a>, <a href="/search/astro-ph?searchtype=author&query=McKay%2C+T+A">T. A. McKay</a>, <a href="/search/astro-ph?searchtype=author&query=Ozel%2C+M">M. Ozel</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+A">A. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Quimby%2C+R+M">R. M. Quimby</a>, <a href="/search/astro-ph?searchtype=author&query=Rowell%2C+G">G. Rowell</a>, <a href="/search/astro-ph?searchtype=author&query=Rujopakarn%2C+W">W. Rujopakarn</a>, <a href="/search/astro-ph?searchtype=author&query=Schaefer%2C+B+E">B. E. Schaefer</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+D+A">D. A. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Swan%2C+H+F">H. F. Swan</a>, <a href="/search/astro-ph?searchtype=author&query=Vestrand%2C+W+T">W. T. Vestrand</a>, <a href="/search/astro-ph?searchtype=author&query=Wheeler%2C+J+C">J. C. Wheeler</a> , et al. (2 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0601350v1-abstract-short" style="display: inline;"> The ROTSE-IIIc telescope at the H.E.S.S. site, Namibia, obtained the earliest detection of optical emission from a Gamma-Ray Burst (GRB), beginning only 21.8 s from the onset of Swift GRB 050801. The optical lightcurve does not fade or brighten significantly over the first ~250 s, after which there is an achromatic break and the lightcurve declines in typical power-law fashion. The Swift/XRT als… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0601350v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0601350v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0601350v1-abstract-full" style="display: none;"> The ROTSE-IIIc telescope at the H.E.S.S. site, Namibia, obtained the earliest detection of optical emission from a Gamma-Ray Burst (GRB), beginning only 21.8 s from the onset of Swift GRB 050801. The optical lightcurve does not fade or brighten significantly over the first ~250 s, after which there is an achromatic break and the lightcurve declines in typical power-law fashion. The Swift/XRT also obtained early observations starting at 69 s after the burst onset. The X-ray lightcurve shows the same features as the optical lightcurve. These correlated variations in the early optical and X-ray emission imply a common origin in space and time. This behavior is difficult to reconcile with the standard models of early afterglow emission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0601350v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0601350v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 January, 2006; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2006. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">5 pages, 1 figure. Accepted for publication in ApJ Letters</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.638:L5-L8,2006 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0511421">arXiv:astro-ph/0511421</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0511421">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0511421">ps</a>, <a href="https://arxiv.org/format/astro-ph/0511421">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/499803">10.1086/499803 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Early-Time Observations of the GRB 050319 Optical Transient </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Quimby%2C+R+M">R. M. Quimby</a>, <a href="/search/astro-ph?searchtype=author&query=Rykoff%2C+E+S">E. S. Rykoff</a>, <a href="/search/astro-ph?searchtype=author&query=Yost%2C+S+A">S. A. Yost</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Alatalo%2C+K">K. Alatalo</a>, <a href="/search/astro-ph?searchtype=author&query=Ashley%2C+M+C+B">M. C. B. Ashley</a>, <a href="/search/astro-ph?searchtype=author&query=Goegues%2C+E">E. Goegues</a>, <a href="/search/astro-ph?searchtype=author&query=Guever%2C+T">T. Guever</a>, <a href="/search/astro-ph?searchtype=author&query=Horns%2C+D">D. Horns</a>, <a href="/search/astro-ph?searchtype=author&query=Kehoe%2C+R+L">R. L. Kehoe</a>, <a href="/search/astro-ph?searchtype=author&query=Kiziloglu%2C+U">Ue. Kiziloglu</a>, <a href="/search/astro-ph?searchtype=author&query=McKay%2C+T+A">T. A. McKay</a>, <a href="/search/astro-ph?searchtype=author&query=Oezel%2C+M">M. Oezel</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+A">A. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Schaefer%2C+B+E">B. E. Schaefer</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+D+A">D. A. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Swan%2C+H+F">H. F. Swan</a>, <a href="/search/astro-ph?searchtype=author&query=Vestrand%2C+W+T">W. T. Vestrand</a>, <a href="/search/astro-ph?searchtype=author&query=Wheeler%2C+J+C">J. C. Wheeler</a>, <a href="/search/astro-ph?searchtype=author&query=Wren%2C+J">J. Wren</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0511421v1-abstract-short" style="display: inline;"> We present the unfiltered ROTSE-III light curve of the optical transient associated with GRB 050319 beginning 4 s after the cessation of gamma-ray activity. We fit a power-law function to the data using the revised trigger time given by Chincarini et al. (2005), and a smoothly broken power-law to the data using the original trigger disseminated through the GCN notices. Including the RAPTOR data… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0511421v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0511421v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0511421v1-abstract-full" style="display: none;"> We present the unfiltered ROTSE-III light curve of the optical transient associated with GRB 050319 beginning 4 s after the cessation of gamma-ray activity. We fit a power-law function to the data using the revised trigger time given by Chincarini et al. (2005), and a smoothly broken power-law to the data using the original trigger disseminated through the GCN notices. Including the RAPTOR data from Wozniak et al. (2005), the best fit power-law indices are alpha=-0.854 (+/- 0.014) for the single power-law and alpha_1=-0.364 (+/- 0.020), alpha_2= -0.881 (+/- 0.030), with a break at t_b = 418 (+/- 30) s for the smoothly broken fit. We discuss the fit results with emphasis placed on the importance of knowing the true start time of the optical transient for this multi-peaked burst. As Swift continues to provide prompt GRB locations, it becomes more important to answer the question, "when does the afterglow begin" to correctly interpret the light curves. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0511421v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0511421v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 November, 2005; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2005. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages including 2 figures; Accepted for publication in ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.640:402-406,2006 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0509594">arXiv:astro-ph/0509594</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0509594">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0509594">ps</a>, <a href="https://arxiv.org/format/astro-ph/0509594">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/498134">10.1086/498134 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Optical Lightcurve & Cooling Break of GRB 050502A </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Yost%2C+S+A">S. A. Yost</a>, <a href="/search/astro-ph?searchtype=author&query=Alatalo%2C+K">K. Alatalo</a>, <a href="/search/astro-ph?searchtype=author&query=Rykoff%2C+E+S">E. S. Rykoff</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Ashley%2C+M+C+B">M. C. B. Ashley</a>, <a href="/search/astro-ph?searchtype=author&query=Blake%2C+C+H">C. H. Blake</a>, <a href="/search/astro-ph?searchtype=author&query=Bloom%2C+J+S">J. S. Bloom</a>, <a href="/search/astro-ph?searchtype=author&query=Boettcher%2C+M">M. Boettcher</a>, <a href="/search/astro-ph?searchtype=author&query=Falco%2C+E+E">E. E. Falco</a>, <a href="/search/astro-ph?searchtype=author&query=Gogus%2C+E">E. Gogus</a>, <a href="/search/astro-ph?searchtype=author&query=Guver%2C+T">T. Guver</a>, <a href="/search/astro-ph?searchtype=author&query=Halpern%2C+J+P">J. P. Halpern</a>, <a href="/search/astro-ph?searchtype=author&query=Horns%2C+D">D. Horns</a>, <a href="/search/astro-ph?searchtype=author&query=Joshi%2C+M">M. Joshi</a>, <a href="/search/astro-ph?searchtype=author&query=Kiziloglu%2C+U">U. Kiziloglu</a>, <a href="/search/astro-ph?searchtype=author&query=McKay%2C+T+A">T. A. McKay</a>, <a href="/search/astro-ph?searchtype=author&query=Mirabal%2C+N">N. Mirabal</a>, <a href="/search/astro-ph?searchtype=author&query=Ozel%2C+M">M. Ozel</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+A">A. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Quimby%2C+R+M">R. M. Quimby</a>, <a href="/search/astro-ph?searchtype=author&query=Rujopakarn%2C+W">W. Rujopakarn</a>, <a href="/search/astro-ph?searchtype=author&query=Schaefer%2C+B+E">B. E. Schaefer</a>, <a href="/search/astro-ph?searchtype=author&query=Shields%2C+J+C">J. C. Shields</a>, <a href="/search/astro-ph?searchtype=author&query=Skrutskie%2C+M">M. Skrutskie</a> , et al. (7 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0509594v1-abstract-short" style="display: inline;"> We present lightcurves of the afterglow of GRB050502A, including very early data at t-t_{GRB} < 60s. The lightcurve is composed of unfiltered ROTSE-IIIb optical observations from 44s to 6h post-burst, R-band MDM observations from 1.6 to 8.4h post-burst, and PAIRITEL J H K_s observations from 0.6 to 2.6h post-burst. The optical lightcurve is fit by a broken power law, where t^{alpha} steepens fro… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0509594v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0509594v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0509594v1-abstract-full" style="display: none;"> We present lightcurves of the afterglow of GRB050502A, including very early data at t-t_{GRB} < 60s. The lightcurve is composed of unfiltered ROTSE-IIIb optical observations from 44s to 6h post-burst, R-band MDM observations from 1.6 to 8.4h post-burst, and PAIRITEL J H K_s observations from 0.6 to 2.6h post-burst. The optical lightcurve is fit by a broken power law, where t^{alpha} steepens from alpha = -1.13 +- 0.02 to alpha = -1.44 +- 0.02 at \~5700s. This steepening is consistent with the evolution expected for the passage of the cooling frequency nu_c through the optical band. Even in our earliest observation at 44s post-burst, there is no evidence that the optical flux is brighter than a backward extrapolation of the later power law would suggest. The observed decay indices and spectral index are consistent with either an ISM or a Wind fireball model, but slightly favor the ISM interpretation. The expected spectral index in the ISM interpretation is consistent within 1 sigma with the observed spectral index beta = -0.8 +- 0.1; the Wind interpretation would imply a slightly (~2 sigma) shallower spectral index than observed. A small amount of dust extinction at the source redshift could steepen an intrinsic spectrum sufficiently to account for the observed value of beta. In this picture, the early optical decay, with the peak at or below 4.7e14 Hz at 44s, requires very small electron and magnetic energy partitions from the fireball. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0509594v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0509594v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 September, 2005; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2005. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, including 3 tables and 1 figure, Accepted by ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.636:959-966,2006 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0509304">arXiv:astro-ph/0509304</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0509304">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0509304">ps</a>, <a href="https://arxiv.org/format/astro-ph/0509304">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/498014">10.1086/498014 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> SN 2005cg: Explosion Physics and Circumstellar Interaction of a Normal Type Ia Supernova in a Low-Luminosity Host </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Quimby%2C+R">Robert Quimby</a>, <a href="/search/astro-ph?searchtype=author&query=Hoeflich%2C+P">Peter Hoeflich</a>, <a href="/search/astro-ph?searchtype=author&query=Kannappan%2C+S+J">Sheila J. Kannappan</a>, <a href="/search/astro-ph?searchtype=author&query=Rykoff%2C+E">Eli Rykoff</a>, <a href="/search/astro-ph?searchtype=author&query=Rujopakarn%2C+W">Wiphu Rujopakarn</a>, <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">Carl W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Gerardy%2C+C+L">Christopher L. Gerardy</a>, <a href="/search/astro-ph?searchtype=author&query=Wheeler%2C+J+C">J. Craig Wheeler</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0509304v1-abstract-short" style="display: inline;"> We present the spectral evolution, light curve, and corresponding interpretation for the "normal-bright" Type Ia Supernova 2005cg discovered by ROTSE-IIIc. The host is a low-luminosity (M_r = -16.75), blue galaxy with strong indications of active star formation and an environment similar to that expected for SNe Ia at high redshifts. Early-time (t ~ -10 days) optical spectra obtained with the HE… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0509304v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0509304v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0509304v1-abstract-full" style="display: none;"> We present the spectral evolution, light curve, and corresponding interpretation for the "normal-bright" Type Ia Supernova 2005cg discovered by ROTSE-IIIc. The host is a low-luminosity (M_r = -16.75), blue galaxy with strong indications of active star formation and an environment similar to that expected for SNe Ia at high redshifts. Early-time (t ~ -10 days) optical spectra obtained with the HET reveal an asymmetric, triangular-shaped Si II absorption feature at about 6100 脜with a sharp transition to the continuum at a blue shift of about 24,000 km s^-1. By 4 days before maximum, the Si II absorption feature becomes symmetric with smoothly curved sides. Similar Si II profile evolution has previously been observed in other supernovae, and is predicted by some explosion models, but its significance has not been fully recognized. Although the spectra predicted by pure deflagration and delayed detonation models are similar near maximum light, they predict qualitatively different chemical abundances in the outer layers and thus give qualitatively different spectra at the earliest phases. The Si line observed in SN 2005cg at early times requires the presence of burning products at high velocities and the triangular shape is likely to be formed in an extended region of slowly declining Si abundance that characterizes delayed detonation models. The spectra show a high-velocity Ca II IR feature that coincides in velocity space with the Si II cutoff. This supports the interpretation that the Ca II is formed when the outer layers of the SN ejecta sweep up about 5 x 10^-3 M_sun of material within the progenitor system. (Abridged) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0509304v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0509304v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 September, 2005; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2005. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">6 pages, Accepted for publication in ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.636:400-405,2005 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0508495">arXiv:astro-ph/0508495</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0508495">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0508495">ps</a>, <a href="https://arxiv.org/format/astro-ph/0508495">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/497370">10.1086/497370 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Prompt Optical Detection of GRB 050401 with ROTSE-IIIa </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rykoff%2C+E+S">E. S. Rykoff</a>, <a href="/search/astro-ph?searchtype=author&query=Yost%2C+S+A">S. A. Yost</a>, <a href="/search/astro-ph?searchtype=author&query=Krimm%2C+H+A">H. A. Krimm</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Alatalo%2C+K">K. Alatalo</a>, <a href="/search/astro-ph?searchtype=author&query=Ashley%2C+M+C+B">M. C. B. Ashley</a>, <a href="/search/astro-ph?searchtype=author&query=Barthelmy%2C+S+D">S. D. Barthelmy</a>, <a href="/search/astro-ph?searchtype=author&query=Gehrels%2C+N">N. Gehrels</a>, <a href="/search/astro-ph?searchtype=author&query=Guver%2C+T">T. Guver</a>, <a href="/search/astro-ph?searchtype=author&query=Horns%2C+D">D. Horns</a>, <a href="/search/astro-ph?searchtype=author&query=Kiziloglu%2C+U">U. Kiziloglu</a>, <a href="/search/astro-ph?searchtype=author&query=McKay%2C+T+A">T. A. McKay</a>, <a href="/search/astro-ph?searchtype=author&query=Ozel%2C+M">M. Ozel</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+A">A. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Quimby%2C+R+M">R. M. Quimby</a>, <a href="/search/astro-ph?searchtype=author&query=Rujopakarn%2C+W">W. Rujopakarn</a>, <a href="/search/astro-ph?searchtype=author&query=Schaefer%2C+B+E">B. E. Schaefer</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+D+A">D. A. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Swan%2C+H+F">H. F. Swan</a>, <a href="/search/astro-ph?searchtype=author&query=Vestrand%2C+W+T">W. T. Vestrand</a>, <a href="/search/astro-ph?searchtype=author&query=Wheeler%2C+J+C">J. C. Wheeler</a>, <a href="/search/astro-ph?searchtype=author&query=Wren%2C+J">J. Wren</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0508495v1-abstract-short" style="display: inline;"> The ROTSE-IIIa telescope at Siding Spring Observatory, Australia, detected prompt optical emission from Swift GRB 050401. In this letter, we present observations of the early optical afterglow, first detected by the ROTSE-IIIa telescope 33 s after the start of gamma-ray emission, contemporaneous with the brightest peak of this emission. This GRB was neither exceptionally long nor bright. This is… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0508495v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0508495v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0508495v1-abstract-full" style="display: none;"> The ROTSE-IIIa telescope at Siding Spring Observatory, Australia, detected prompt optical emission from Swift GRB 050401. In this letter, we present observations of the early optical afterglow, first detected by the ROTSE-IIIa telescope 33 s after the start of gamma-ray emission, contemporaneous with the brightest peak of this emission. This GRB was neither exceptionally long nor bright. This is the first prompt optical detection of a GRB of typical duration and luminosity. We find that the early afterglow decay does not deviate significantly from the power-law decay observable at later times, and is uncorrelated with the prompt gamma-ray emission. We compare this detection with the other two GRBs with prompt observations, GRB 990123 and GRB 041219a. All three bursts exhibit quite different behavior at early times. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0508495v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0508495v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 August, 2005; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2005. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">4 pages, 3 figures. Accepted for publication in ApJ Letters</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.631:L121-L124,2005 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0506442">arXiv:astro-ph/0506442</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0506442">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0506442">ps</a>, <a href="https://arxiv.org/format/astro-ph/0506442">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/432832">10.1086/432832 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Search for Untriggered GRB Afterglows with ROTSE-III </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rykoff%2C+E+S">E. S. Rykoff</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Alatalo%2C+K">K. Alatalo</a>, <a href="/search/astro-ph?searchtype=author&query=Ashley%2C+M+C+B">M. C. B. Ashley</a>, <a href="/search/astro-ph?searchtype=author&query=Guver%2C+T">T. Guver</a>, <a href="/search/astro-ph?searchtype=author&query=Horns%2C+D">D. Horns</a>, <a href="/search/astro-ph?searchtype=author&query=Kehoe%2C+R+L">R. L. Kehoe</a>, <a href="/search/astro-ph?searchtype=author&query=Kiziloglu%2C+U">U. Kiziloglu</a>, <a href="/search/astro-ph?searchtype=author&query=McKay%2C+T+A">T. A. McKay</a>, <a href="/search/astro-ph?searchtype=author&query=Ozel%2C+M">M. Ozel</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+A">A. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Quimby%2C+R+M">R. M. Quimby</a>, <a href="/search/astro-ph?searchtype=author&query=Schaefer%2C+B+E">B. E. Schaefer</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+D+A">D. A. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Swan%2C+H+F">H. F. Swan</a>, <a href="/search/astro-ph?searchtype=author&query=Vestrand%2C+W+T">W. T. Vestrand</a>, <a href="/search/astro-ph?searchtype=author&query=Wheeler%2C+J+C">J. C. Wheeler</a>, <a href="/search/astro-ph?searchtype=author&query=Wren%2C+J">J. Wren</a>, <a href="/search/astro-ph?searchtype=author&query=Yost%2C+S+A">S. A. Yost</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0506442v1-abstract-short" style="display: inline;"> We present the results of a search for untriggered gamma-ray burst (GRB) afterglows with the Robotic Optical Transient Search Experiment-III (ROTSE-III) telescope array. This search covers observations from September 2003 to March 2005. We have an effective coverage of 1.74 deg^2 yr for rapidly fading transients that remain brighter than ~ 17.5 magnitude for more than 30 minutes. This search is… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0506442v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0506442v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0506442v1-abstract-full" style="display: none;"> We present the results of a search for untriggered gamma-ray burst (GRB) afterglows with the Robotic Optical Transient Search Experiment-III (ROTSE-III) telescope array. This search covers observations from September 2003 to March 2005. We have an effective coverage of 1.74 deg^2 yr for rapidly fading transients that remain brighter than ~ 17.5 magnitude for more than 30 minutes. This search is the first large area survey to be able to detect typical untriggered GRB afterglows. Our background rate is very low and purely astrophysical. We have found 4 previously unknown cataclysmic variables (CVs) and 1 new flare star. We have not detected any candidate afterglow events or other unidentified transients. We can place an upper limit on the rate of fading optical transients with quiescent counterparts dimmer than ~ 20th magnitude at a rate of less than 1.9 deg^-2 yr-1 with 95% confidence. This places limits on the optical characteristics of off-axis (orphan) GRB afterglows. As a byproduct of this search, we have an effective ~ 52 deg^2 yr of coverage for very slowly decaying transients, such as CVs. This implies an overall rate of outbursts from high galactic latitude CVs of 0.1 deg^2 yr^-1. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0506442v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0506442v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 June, 2005; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2005. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Seven pages, five figures, uses emulateapj class file. Accepted to Astrophysical Journal</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.631:1032-1038,2005 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0401217">arXiv:astro-ph/0401217</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0401217">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0401217">ps</a>, <a href="https://arxiv.org/format/astro-ph/0401217">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/382719">10.1086/382719 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Northern Sky Variability Survey (NSVS): Public data release </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wozniak%2C+P+R">P. R. Wozniak</a>, <a href="/search/astro-ph?searchtype=author&query=Vestrand%2C+W+T">W. T. Vestrand</a>, <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Balsano%2C+R">R. Balsano</a>, <a href="/search/astro-ph?searchtype=author&query=Bloch%2C+J">J. Bloch</a>, <a href="/search/astro-ph?searchtype=author&query=Casperson%2C+D">D. Casperson</a>, <a href="/search/astro-ph?searchtype=author&query=Fletcher%2C+S">S. Fletcher</a>, <a href="/search/astro-ph?searchtype=author&query=Gisler%2C+G">G. Gisler</a>, <a href="/search/astro-ph?searchtype=author&query=Kehoe%2C+R">R. Kehoe</a>, <a href="/search/astro-ph?searchtype=author&query=Kinemuchi%2C+K">K. Kinemuchi</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+B+C">B. C. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Marshall%2C+S">S. Marshall</a>, <a href="/search/astro-ph?searchtype=author&query=McGowan%2C+K+E">K. E. McGowan</a>, <a href="/search/astro-ph?searchtype=author&query=McKay%2C+T+A">T. A. McKay</a>, <a href="/search/astro-ph?searchtype=author&query=Rykoff%2C+E+S">E. S. Rykoff</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+D+A">D. A. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Szymanski%2C+J">J. Szymanski</a>, <a href="/search/astro-ph?searchtype=author&query=Wren%2C+J">J. Wren</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0401217v1-abstract-short" style="display: inline;"> The Northern Sky Variability Survey (NSVS) is a temporal record of the sky over the optical magnitude range from 8 to 15.5. It was conducted in the course of the first generation Robotic Optical Transient Search Experiment (ROTSE-I) using a robotic system of four co-mounted unfiltered telephoto lenses equipped with CCD cameras. The survey was conducted from Los Alamos, NM, and primarily covers t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0401217v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0401217v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0401217v1-abstract-full" style="display: none;"> The Northern Sky Variability Survey (NSVS) is a temporal record of the sky over the optical magnitude range from 8 to 15.5. It was conducted in the course of the first generation Robotic Optical Transient Search Experiment (ROTSE-I) using a robotic system of four co-mounted unfiltered telephoto lenses equipped with CCD cameras. The survey was conducted from Los Alamos, NM, and primarily covers the entire northern sky. Some data in southern fields between declinations 0 and -38 deg is also available, although with fewer epochs and noticeably lesser quality. The NSVS contains light curves for approximately 14 million objects. With a one year baseline and typically 100-500 measurements per object, the NSVS is the most extensive record of stellar variability across the bright sky available today. In a median field, bright unsaturated stars attain a point to point photometric scatter of ~0.02 mag and position errors within 2 arcsec. At Galactic latitudes |b| < 20 deg the data quality is limited by severe blending due to ~14 arcsec pixel size. We present basic characteristics of the data set and describe data collection, analysis, and distribution. All NSVS photometric measurements are available for on-line public access from the Sky Database for Objects in Time-Domain (SkyDOT; http://skydot.lanl.gov) at LANL. Copies of the full survey photometry may also be requested on tape. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0401217v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0401217v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 January, 2004; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2004. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted for publication in Astronomical Journal</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LAUR-03-8792 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astron.J.127:2436-2449,2004 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0310501">arXiv:astro-ph/0310501</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0310501">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0310501">ps</a>, <a href="https://arxiv.org/format/astro-ph/0310501">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/380777">10.1086/380777 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Early Optical Afterglow of GRB 030418 and Progenitor Mass Loss </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rykoff%2C+E+S">E. S. Rykoff</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+D+A">D. A. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Price%2C+P+A">P. A. Price</a>, <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Ashley%2C+M+C+B">M. C. B. Ashley</a>, <a href="/search/astro-ph?searchtype=author&query=Bizyaev%2C+D">D. Bizyaev</a>, <a href="/search/astro-ph?searchtype=author&query=Garradd%2C+G+J">G. J. Garradd</a>, <a href="/search/astro-ph?searchtype=author&query=McKay%2C+T+A">T. A. McKay</a>, <a href="/search/astro-ph?searchtype=author&query=McNaught%2C+R+H">R. H. McNaught</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+A">A. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Quimby%2C+R">R. Quimby</a>, <a href="/search/astro-ph?searchtype=author&query=Schaefer%2C+B">B. Schaefer</a>, <a href="/search/astro-ph?searchtype=author&query=Schmidt%2C+B">B. Schmidt</a>, <a href="/search/astro-ph?searchtype=author&query=Vestrand%2C+W+T">W. T. Vestrand</a>, <a href="/search/astro-ph?searchtype=author&query=Wheeler%2C+J+C">J. C. Wheeler</a>, <a href="/search/astro-ph?searchtype=author&query=Wren%2C+J">J. Wren</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0310501v1-abstract-short" style="display: inline;"> The ROTSE-IIIa telescope and the SSO-40 inch telescope, both located at Siding Spring Observatory, imaged the early time afterglow of GRB 030418. In this report we present observations of the early afterglow, first detected by the ROTSE-IIIa telescope 211 s after the start of the burst, and only 76 s after the end of the gamma-ray activity. We detect optical emission that rises for ~600 s, slowl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0310501v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0310501v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0310501v1-abstract-full" style="display: none;"> The ROTSE-IIIa telescope and the SSO-40 inch telescope, both located at Siding Spring Observatory, imaged the early time afterglow of GRB 030418. In this report we present observations of the early afterglow, first detected by the ROTSE-IIIa telescope 211 s after the start of the burst, and only 76 s after the end of the gamma-ray activity. We detect optical emission that rises for ~600 s, slowly varies around R=17.3 mag for ~1400 s, and then fades as a power law of index alpha=-1.36. Additionally, the ROTSE-IIIb telescope, located at McDonald Observatory, imaged the early time afterglow of GRB 030723. The behavior of this light curve was qualitatively similar to that of GRB 030418, but two magnitudes dimmer. These two afterglows are dissimilar to other afterglows such as GRB 990123 and GRB 021211. We investigate whether the early afterglow can be attributed to a synchrotron break in a cooling synchrotron spectrum as it passes through the optical band, but find this model is unable to accurately describe the early light curve. We present a simple model for gamma-ray burst emission emerging from a wind medium surrounding a massive progenitor star. This model provides an effective description of the data, and suggests that the rise of the afterglow can be ascribed to extinction in the local circumburst environment. In this interpretation, these events provide further evidence for the connection between gamma-ray bursts and the collapse of massive stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0310501v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0310501v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 October, 2003; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2003. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Five pages, four figures, uses emulateapj class file. Accepted to Astrophysical Journal Letters</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J. 601 (2004) 1013-1018 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0309177">arXiv:astro-ph/0309177</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0309177">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0309177">ps</a>, <a href="https://arxiv.org/format/astro-ph/0309177">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/379534">10.1086/379534 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> ROTSE-III Observations of the Early Afterglow From GRB 030329 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Smith%2C+D+A">D. A. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Rykoff%2C+E+S">E. S. Rykoff</a>, <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Ashley%2C+M+C+B">M. C. B. Ashley</a>, <a href="/search/astro-ph?searchtype=author&query=Bizyaev%2C+D">D. Bizyaev</a>, <a href="/search/astro-ph?searchtype=author&query=McKay%2C+T+A">T. A. McKay</a>, <a href="/search/astro-ph?searchtype=author&query=Mukadum%2C+A">A. Mukadum</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+A">A. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Quimby%2C+R">R. Quimby</a>, <a href="/search/astro-ph?searchtype=author&query=Schaefer%2C+B">B. Schaefer</a>, <a href="/search/astro-ph?searchtype=author&query=Sullivan%2C+D">D. Sullivan</a>, <a href="/search/astro-ph?searchtype=author&query=Swan%2C+H+F">H. F. Swan</a>, <a href="/search/astro-ph?searchtype=author&query=Vestrand%2C+W+T">W. T. Vestrand</a>, <a href="/search/astro-ph?searchtype=author&query=Wheeler%2C+J+C">J. C. Wheeler</a>, <a href="/search/astro-ph?searchtype=author&query=Wren%2C+J">J. Wren</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0309177v1-abstract-short" style="display: inline;"> Using two identical telescopes at widely separated longitudes, the ROTSE-III network observed decaying emission from the remarkably bright afterglow of GRB 030329. In this report we present observations covering 56% of the period from 1.5-47 hours after the burst. We find that the light curve is piecewise consistent with a powerlaw decay. When the ROTSE-III data are combined with data reported b… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0309177v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0309177v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0309177v1-abstract-full" style="display: none;"> Using two identical telescopes at widely separated longitudes, the ROTSE-III network observed decaying emission from the remarkably bright afterglow of GRB 030329. In this report we present observations covering 56% of the period from 1.5-47 hours after the burst. We find that the light curve is piecewise consistent with a powerlaw decay. When the ROTSE-III data are combined with data reported by other groups, there is evidence for five breaks within the first 20 hours after the burst. Between two of those breaks, observations from 15.9-17.1 h after the burst at 1-s time resolution with McDonald Observatory's 2.1-m telescope reveal no evidence for fluctuations or deviations from a simple power law. Multiple breaks may indicate complex structure in the jet. There are also two unambiguous episodes at 23 and 45 hours after the burst where the intensity becomes consistent with a constant for several hours, perhaps indicating multiple injections of energy into the GRB/afterglow system. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0309177v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0309177v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 September, 2003; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2003. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Four pages, two figures, uses emulateapj class file. Accepted to Astrophysical Journal Letters</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.596:L151-L154,2003 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0210238">arXiv:astro-ph/0210238</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0210238">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0210238">ps</a>, <a href="https://arxiv.org/format/astro-ph/0210238">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/345490">10.1086/345490 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The ROTSE-III Robotic Telescope System </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Ashley%2C+M+C+B">M. C. B. Ashley</a>, <a href="/search/astro-ph?searchtype=author&query=Casperson%2C+D+E">D. E. Casperson</a>, <a href="/search/astro-ph?searchtype=author&query=Epps%2C+H+W">H. W. Epps</a>, <a href="/search/astro-ph?searchtype=author&query=Kehoe%2C+R+L">R. L. Kehoe</a>, <a href="/search/astro-ph?searchtype=author&query=Marshall%2C+S+L">S. L. Marshall</a>, <a href="/search/astro-ph?searchtype=author&query=McGowan%2C+K+E">K. E. McGowan</a>, <a href="/search/astro-ph?searchtype=author&query=McKay%2C+T+A">T. A. McKay</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+M+A">M. A. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Rykoff%2C+E+S">E. S. Rykoff</a>, <a href="/search/astro-ph?searchtype=author&query=Schier%2C+J+A">J. A. Schier</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+D+A">D. A. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Vestrand%2C+W+T">W. T. Vestrand</a>, <a href="/search/astro-ph?searchtype=author&query=Wozniak%2C+P+R">P. R. Wozniak</a>, <a href="/search/astro-ph?searchtype=author&query=Wren%2C+J+A">J. A. Wren</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0210238v1-abstract-short" style="display: inline;"> The observation of a prompt optical flash from GRB990123 convincingly demonstrated the value of autonomous robotic telescope systems. Pursuing a program of rapid follow-up observations of gamma-ray bursts, the Robotic Optical Transient Search Experiment (ROTSE) has developed a next-generation instrument, ROTSE-III, that will continue the search for fast optical transients. The entire system was… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0210238v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0210238v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0210238v1-abstract-full" style="display: none;"> The observation of a prompt optical flash from GRB990123 convincingly demonstrated the value of autonomous robotic telescope systems. Pursuing a program of rapid follow-up observations of gamma-ray bursts, the Robotic Optical Transient Search Experiment (ROTSE) has developed a next-generation instrument, ROTSE-III, that will continue the search for fast optical transients. The entire system was designed as an economical robotic facility to be installed at remote sites throughout the world. There are seven major system components: optics, optical tube assembly, CCD camera, telescope mount, enclosure, environmental sensing & protection and data acquisition. Each is described in turn in the hope that the techniques developed here will be useful in similar contexts elsewhere. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0210238v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0210238v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 October, 2002; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2002. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, including 4 figures. To be published in PASP in January, 2003. PASP Number IP02-110</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/9712325">arXiv:astro-ph/9712325</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/9712325">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/9712325">ps</a>, <a href="https://arxiv.org/format/astro-ph/9712325">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/305857">10.1086/305857 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery of >350 GeV Gamma Rays from the BL Lacertae Object 1ES 2344+514 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Catanese%2C+M">M. Catanese</a>, <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Badran%2C+H+M">H. M. Badran</a>, <a href="/search/astro-ph?searchtype=author&query=Biller%2C+S+D">S. D. Biller</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+I+H">I. H. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Boyle%2C+P+J">P. J. Boyle</a>, <a href="/search/astro-ph?searchtype=author&query=Bradbury%2C+S+M">S. M. Bradbury</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+J+H">J. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Burdett%2C+A+M">A. M. Burdett</a>, <a href="/search/astro-ph?searchtype=author&query=Gordo%2C+J+B">J. Bussons Gordo</a>, <a href="/search/astro-ph?searchtype=author&query=Carter-Lewis%2C+D+A">D. A. Carter-Lewis</a>, <a href="/search/astro-ph?searchtype=author&query=Cawley%2C+M+F">M. F. Cawley</a>, <a href="/search/astro-ph?searchtype=author&query=Connaughton%2C+V">V. Connaughton</a>, <a href="/search/astro-ph?searchtype=author&query=Fegan%2C+D+J">D. J. Fegan</a>, <a href="/search/astro-ph?searchtype=author&query=Finley%2C+J+P">J. P. Finley</a>, <a href="/search/astro-ph?searchtype=author&query=Gaidos%2C+J+A">J. A. Gaidos</a>, <a href="/search/astro-ph?searchtype=author&query=Hall%2C+T">T. Hall</a>, <a href="/search/astro-ph?searchtype=author&query=Hillas%2C+A+M">A. M. Hillas</a>, <a href="/search/astro-ph?searchtype=author&query=Krennrich%2C+F">F. Krennrich</a>, <a href="/search/astro-ph?searchtype=author&query=Lamb%2C+R+C">R. C. Lamb</a>, <a href="/search/astro-ph?searchtype=author&query=Lessard%2C+R+W">R. W. Lessard</a>, <a href="/search/astro-ph?searchtype=author&query=Masterson%2C+C">C. Masterson</a>, <a href="/search/astro-ph?searchtype=author&query=McEnery%2C+J+E">J. E. McEnery</a>, <a href="/search/astro-ph?searchtype=author&query=Mohanty%2C+G">G. Mohanty</a>, <a href="/search/astro-ph?searchtype=author&query=Quinn%2C+J">J. Quinn</a> , et al. (9 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/9712325v1-abstract-short" style="display: inline;"> We present the discovery of >350 GeV gamma-ray emission from the BL Lacertae object 1ES 2344+514 with the Whipple Observatory 10m gamma-ray telescope. This is the third BL Lac object detected at gamma-ray energies above 300 Gev, the other two being Markarian 421 (Mrk 421) and Mrk501. These three active galactic nuclei are all X-ray selected and have the lowest known redshifts of any BL Lac objec… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9712325v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/9712325v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/9712325v1-abstract-full" style="display: none;"> We present the discovery of >350 GeV gamma-ray emission from the BL Lacertae object 1ES 2344+514 with the Whipple Observatory 10m gamma-ray telescope. This is the third BL Lac object detected at gamma-ray energies above 300 Gev, the other two being Markarian 421 (Mrk 421) and Mrk501. These three active galactic nuclei are all X-ray selected and have the lowest known redshifts of any BL Lac objects currently identified. The evidence for emission derives primarily from an apparent flare on December 20, 1995 when a 6 sigma excess was detected with a flux approximately 63% of the very high energy gamma-ray emission from the Crab Nebula, the standard candle for TeV gamma-ray sources. Excluding the flare, observations between October 1995 and January 1996 yield a 4 sigma detection corresponding to 11% of the VHE Crab Nebula flux. Observations spanning September 1996 to January 1997 failed to yield a significant detection of a steady flux or any flaring. For this period, the 99.9% confidence level upper limit is <8% of the Crab Nebula. The low baseline emission level and variations in nightly and yearly flux of 1ES 22344+514 are the same as the VHE emission characteristics of Mrk 421 and Mrk 501 <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9712325v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/9712325v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 December, 1997; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 1997. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 6 Postscript figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FLWO-97-12-1 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.501:616-623,1998 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/9706123">arXiv:astro-ph/9706123</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/9706123">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/9706123">ps</a>, <a href="https://arxiv.org/format/astro-ph/9706123">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/367825">10.1086/367825 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A search for correlations of TeV gamma-rays with ultra-high energy cosmic rays </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Biller%2C+S">S. Biller</a>, <a href="/search/astro-ph?searchtype=author&query=Boyle%2C+P">P. Boyle</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+J">J. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Carter-Lewis%2C+D+A">D. A. Carter-Lewis</a>, <a href="/search/astro-ph?searchtype=author&query=Catanese%2C+M">M. Catanese</a>, <a href="/search/astro-ph?searchtype=author&query=Cawley%2C+M+F">M. F. Cawley</a>, <a href="/search/astro-ph?searchtype=author&query=Connaughton%2C+V">V. Connaughton</a>, <a href="/search/astro-ph?searchtype=author&query=Fegan%2C+D+J">D. J. Fegan</a>, <a href="/search/astro-ph?searchtype=author&query=Finley%2C+J">J. Finley</a>, <a href="/search/astro-ph?searchtype=author&query=Gaidos%2C+J">J. Gaidos</a>, <a href="/search/astro-ph?searchtype=author&query=Hillas%2C+A+M">A. M. Hillas</a>, <a href="/search/astro-ph?searchtype=author&query=Krennrich%2C+F">F. Krennrich</a>, <a href="/search/astro-ph?searchtype=author&query=Lamb%2C+R+C">R. C. Lamb</a>, <a href="/search/astro-ph?searchtype=author&query=Lessard%2C+R">R. Lessard</a>, <a href="/search/astro-ph?searchtype=author&query=McEnery%2C+J">J. McEnery</a>, <a href="/search/astro-ph?searchtype=author&query=Mohanty%2C+G">G. Mohanty</a>, <a href="/search/astro-ph?searchtype=author&query=Porter%2C+N+A">N. A. Porter</a>, <a href="/search/astro-ph?searchtype=author&query=Quinn%2C+J">J. Quinn</a>, <a href="/search/astro-ph?searchtype=author&query=Rodgers%2C+A">A. Rodgers</a>, <a href="/search/astro-ph?searchtype=author&query=Rose%2C+H+J">H. J. Rose</a>, <a href="/search/astro-ph?searchtype=author&query=Samuelson%2C+F">F. Samuelson</a>, <a href="/search/astro-ph?searchtype=author&query=Schubnell%2C+M+S">M. S. Schubnell</a>, <a href="/search/astro-ph?searchtype=author&query=Sembroski%2C+G">G. Sembroski</a>, <a href="/search/astro-ph?searchtype=author&query=Srinivasan%2C+R">R. Srinivasan</a> , et al. (3 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/9706123v1-abstract-short" style="display: inline;"> A search was conducted for TeV gamma-rays emitted from the direction of the ultra-high energy cosmic ray detected by the Fly's Eye Experiment with E ~ 3 x 10**20 eV. No enhancement was found at a level of 10**-10 gamma/cm**2-sec for E>350 GeV. This upper limit is consistent with theoretical estimates based on topological defects as sources of UHE cosmic rays. An upper limit was also set for the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9706123v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/9706123v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/9706123v1-abstract-full" style="display: none;"> A search was conducted for TeV gamma-rays emitted from the direction of the ultra-high energy cosmic ray detected by the Fly's Eye Experiment with E ~ 3 x 10**20 eV. No enhancement was found at a level of 10**-10 gamma/cm**2-sec for E>350 GeV. This upper limit is consistent with theoretical estimates based on topological defects as sources of UHE cosmic rays. An upper limit was also set for the flux of TeV gamma rays from 3C147, the most prominent AGN in the error box. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9706123v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/9706123v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 June, 1997; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 1997. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 4 figures, Latex with AAS macros, submitted to ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J. 586 (2003) 1232-1237 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/9602068">arXiv:astro-ph/9602068</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/9602068">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/9602068">ps</a>, <a href="https://arxiv.org/format/astro-ph/9602068">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/176998">10.1086/176998 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Very High Energy Gamma-Ray Emission from the Blazar Markarian 421 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Schubnell%2C+M+S">M. S. Schubnell</a>, <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+S+B+J">S. Biller J. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Carter-Lewis%2C+D+A">D. A. Carter-Lewis</a>, <a href="/search/astro-ph?searchtype=author&query=Cawley%2C+M+F">M. F. Cawley</a>, <a href="/search/astro-ph?searchtype=author&query=Chantell%2C+M">M. Chantell</a>, <a href="/search/astro-ph?searchtype=author&query=Connaughton%2C+V">V. Connaughton</a>, <a href="/search/astro-ph?searchtype=author&query=Fegan%2C+D+J">D. J. Fegan</a>, <a href="/search/astro-ph?searchtype=author&query=Fennell%2C+S">S. Fennell</a>, <a href="/search/astro-ph?searchtype=author&query=Gaidos%2C+J+A">J. A. Gaidos</a>, <a href="/search/astro-ph?searchtype=author&query=Hillas%2C+A+M">A. M. Hillas</a>, <a href="/search/astro-ph?searchtype=author&query=Lamb%2C+A+D+K+R+C">A. D. Kerrick R. C. Lamb</a>, <a href="/search/astro-ph?searchtype=author&query=Meyer%2C+D+I">D. I. Meyer</a>, <a href="/search/astro-ph?searchtype=author&query=Mohanty%2C+G">G. Mohanty</a>, <a href="/search/astro-ph?searchtype=author&query=Rose%2C+J">J. Rose</a>, <a href="/search/astro-ph?searchtype=author&query=Rovero%2C+A+C">A. C. Rovero</a>, <a href="/search/astro-ph?searchtype=author&query=Sembroski%2C+G">G. Sembroski</a>, <a href="/search/astro-ph?searchtype=author&query=Weekes%2C+T+C">T. C. Weekes</a>, <a href="/search/astro-ph?searchtype=author&query=Wilson%2C+C">C. Wilson</a>, <a href="/search/astro-ph?searchtype=author&query=Zweerink%2C+J">J. Zweerink</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/9602068v1-abstract-short" style="display: inline;"> Very high energy gamma-ray emission from the BL Lac object Markarian 421 has been detected over three observing seasons on 59 nights between April 1992 and June 1994 with the Whipple 10-meter imaging Cherenkov telescope. During its initial detection in 1992, its flux above 500 GeV was 1.6$\times$10$^{-11}$photons cm$^{-2}$ s$^{-1}$. Observations in 1993 confirmed this level of emission. For obse… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9602068v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/9602068v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/9602068v1-abstract-full" style="display: none;"> Very high energy gamma-ray emission from the BL Lac object Markarian 421 has been detected over three observing seasons on 59 nights between April 1992 and June 1994 with the Whipple 10-meter imaging Cherenkov telescope. During its initial detection in 1992, its flux above 500 GeV was 1.6$\times$10$^{-11}$photons cm$^{-2}$ s$^{-1}$. Observations in 1993 confirmed this level of emission. For observations made between December 1993 and April 1994, its intensity was a factor of 2.2$\pm$0.5 lower. Observations on 14 and 15 May, 1994 showed an increase over this quiescent level by a factor of $\sim$10 (Kerrick et al. 1995). This strong outburst suggests that 4 episodes of increased flux measurements on similar time scales in 1992 and 1994 may be attributed to somewhat weaker outbursts. The variability of the TeV gamma-ray emission from Markarian 421 stands in contrast to EGRET observations (Lin et al. 1994) which show no evidence for variability. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9602068v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/9602068v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 February, 1996; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 1996. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">gzip compressed tar file including LaTeX text and 4 postscript figures (14 pages total incl. 4 tables), accepted for publication in the Astrophysical Journal. Contact address is schubnel@umich.edu</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/9309052">arXiv:astro-ph/9309052</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/9309052">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/9309052">ps</a>, <a href="https://arxiv.org/format/astro-ph/9309052">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1038/365621a0">10.1038/365621a0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Possible Gravitational Microlensing of a Star in the Large Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Alcock%2C+C">C. Alcock</a>, <a href="/search/astro-ph?searchtype=author&query=Akerlof%2C+C+W">C. W. Akerlof</a>, <a href="/search/astro-ph?searchtype=author&query=Allsman%2C+R+A">R. A. Allsman</a>, <a href="/search/astro-ph?searchtype=author&query=Axelrod%2C+T+S">T. S. Axelrod</a>, <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+D+P">D. P. Bennett</a>, <a href="/search/astro-ph?searchtype=author&query=Chan%2C+S">S. Chan</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+K+H">K. H. Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Freeman%2C+K+C">K. C. Freeman</a>, <a href="/search/astro-ph?searchtype=author&query=Griest%2C+K">K. Griest</a>, <a href="/search/astro-ph?searchtype=author&query=Marshall%2C+S+L">S. L. Marshall</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+H">H-S. Park</a>, <a href="/search/astro-ph?searchtype=author&query=Perlmutter%2C+S">S. Perlmutter</a>, <a href="/search/astro-ph?searchtype=author&query=Peterson%2C+B+A">B. A. Peterson</a>, <a href="/search/astro-ph?searchtype=author&query=Pratt%2C+M+R">M. R. Pratt</a>, <a href="/search/astro-ph?searchtype=author&query=Quinn%2C+P+J">P. J. Quinn</a>, <a href="/search/astro-ph?searchtype=author&query=Rodgers%2C+A+W">A. W. Rodgers</a>, <a href="/search/astro-ph?searchtype=author&query=Stubbs%2C+C+W">C. W. Stubbs</a>, <a href="/search/astro-ph?searchtype=author&query=Sutherland%2C+W">W. Sutherland</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/9309052v1-abstract-short" style="display: inline;"> There is now abundant evidence for the presence of large quantities of unseen matter surrounding normal galaxies, including our own$^{1,2}$. The nature of this `dark matter' is unknown, except that it cannot be made of normal stars, dust, or gas, as they would be easily detected. Exotic particles such as axions, massive neutrinos or other weakly interacting massive particles (collectively known… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9309052v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/9309052v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/9309052v1-abstract-full" style="display: none;"> There is now abundant evidence for the presence of large quantities of unseen matter surrounding normal galaxies, including our own$^{1,2}$. The nature of this `dark matter' is unknown, except that it cannot be made of normal stars, dust, or gas, as they would be easily detected. Exotic particles such as axions, massive neutrinos or other weakly interacting massive particles (collectively known as WIMPs) have been proposed)$^{3,4}$, but have yet to be detected. A less exotic alternative is normal matter in the form of bodies with masses ranging from that of a large planet to a few $ \msun$. Such objects, known collectively as massive compact halo objects$^5$ (MACHOs) might be brown dwarfs or `Jupiters' (bodies too small to produce their own energy by fusion), neutron stars, old white dwarfs, or black holes. Paczynski$^6$ suggested that MACHOs might act as gravitational microlenses, occasionally causing the apparent brightness of distant background stars temporarily to increase. We are conducting a microlensing experiment to determine whether the dark matter halo of our galaxy is made up of MACHOs. Here we report a candidate for a microlensing event, detected by monitoring the light curves of 1.8 million stars in the Large Magellanic Cloud for one year. The light curve shows no variation for most of the year of data taking, and an upward excursion lasting over 1 month, with a maximum increase of $\approx \bf 2$ mag. The most probable lens mass, inferred from the duration of the event, is $\bf \sim 0.1 \,\msun$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9309052v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/9309052v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 September, 1993; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 1993. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">plainTeX, 5 pages, 3 figures uunecoded tar-compressed, CFPA-preprint-93-30</span> </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 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